present and future of pulsar research: the italian contribute alessandro corongiu ligo-g060286-00-z...
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Present and future of pulsar research: the Italian
contribute
Alessandro Corongiu
LIGO-G060286-00-Z
Gravitational Waves Advanced Detectors Workshop
La Biodola – Isola d’Elba
Monday May 29th, 2006
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OUTLINE
• The Italian Pulsar Group
• Pulsars
• Current Activities
• SRT
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The Italian Pulsar Group
Istituto Nazionale di AstroFisica
Università degli Studi di Cagliari
Member of VESF
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The Italian Pulsar GroupHead:
Prof. N. D’Amico (OAC Director)
Full time researchers:
Dr. M. Burgay Dr. A. Possenti
Post-doctoral fellows:
Dr. A. Corongiu
Technical support:
A. Fara
Undergraduate students:
M. Bachetti N. Iacolina M. Pierbattista
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PulsarsHigly magnetised and rapidly rotating neutron stars
Pulsars behave like very precise cosmic clocks!!!!
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Pulses’ time of arrival (ToA)
Times of arrival are determined by the convolution of the observed pulse’s profile to a pulse’s temlplate.
Typical uncertainties depend on:- pulsar period- pulse’s width- signal to noise ratio
For millisecond pulsars ToA’s uncertainty can be as small as:
σ 1 μs
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Pulsar timing
Fit procedure of all collected ToAs to a kinematical model.
A timing model is a set of measurable parameters:
• Rotation parameters
• Astrometric parameters
• Keplerian parameters
• Post Keplerian parameters
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Pulsar Projects @ Cagliari
Pulsar projects at Cagliari can be grouped in two (obvious)
groups:
• Survey Projects, to find out as much pulsar as possible
• Timing Projects, to extract from known pulsars as much informations as possible.
Observations are carried out with the Parkes Radio
Telescope (AU).
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The Parkes Telescope
32° 59' 59".8657 Latitude South 391.79 m a.s.l.148° 15' 44".3591 Longitude East 64 m diameter
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Multibeam receiver13 receivers in one to observe towards13 different directions at onceSurvey projects become 13 times faster.
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Survey projects
• Parkes Multibeam Pulsar Survey (completed)• Parkes High Latitude Pulsar Survey (completed)• Perseus Arm Pulsar Survey (in progress)• Parkes Methanol Pulsar Survey (just started)• Globular Clusters’ Pulsars Search (in progress)
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Parkes Surveys: Sky coverage
b (°)
l (°)
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Survey projects
l
(deg)
b
(deg)
Freq.
(MHz)
Bandwidth
(ch x chwidth x npol)
Sampl
rate
(ms)
Int
Time
(min)
PM -100 < l < 50 -5 < b < 5 1374 288
(96 x 3 x 2)
0.25
(1 bit)
35
PH 220 < l < 260 -60 < b < 60 1374 288
(96 x 3 x 2)
0.25
(1 bit)
35
PA 200 < l < 260 -5 < b < 5 1374 288
(96 x 3 x 2)
0.125
(1 bit)
35
METH -25 < l < 25 -1 < b < 1 6410 576
(192 x 3 x 2)
0.25
(1 bit)
70/140
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MANGUSTA
MultiprocessorArray forNewGenerationpUlsar Searched andTimingAnalysis
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Pulsar Population
• 1627 Pulsars known
• 101 in Globular Clusters
• 20 in Magellanic Clouds
• 11 RRATS
• 124 Binaries
8 Double neutron star binaries
• 1 Double pulsar binary
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Timing projects
• Timing of pulsars discovered in all aforementioned surveys.
• Timing of pulsars in globular clusters.
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PSR B PSR D
PSR E
PSR C
PSR A
NGC 6752: Two pulsars at unusual positions and moving very
fast!
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NGC 6752: Open questions
• The high value for the line-of-sight acceleration for the central pulsars indicates a cluster core with a very high mass-to-light ratio.
• The high values for the transverse velocity of the outher pulsars indicate a cluster whose global mass-to-light ratio is too high for a globular cluster.
• There is a hint for the presence of an intermediate mass binary balck hole (10 and 50 M), which may be a source of detectable GWs.
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PSR J1740-5340 in NGC 6397
• PSR J1740-5340 is a newly born millisecond pulsar.
• Radio and X-ray observations allow to investigate the physics of neutron star in accreting binaries.
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PSR J1740-5340 in NGC 6397
• Binaries that produce millisecond pulsars in globular clusters are formation through casual encounters in the cluster’s core.
• Some of such systems are very close and are not observable as radio pulsar because of eclipses due to the accreting matter. They may be sources of detectable GW.
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PSR J0737-3039A/Ba.k.a. : the double pulsar
• It is the most relativistic binary pulsar known to date. Its discovery increased of a factor 5-10 the expected rate of coalescing binaries.
• Three years of regular timing observations have lead to the measure of 5 post-keplerian parameters… and with the highest precision!
• Within reasonable time second order PK parameters are espected to be measured.
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The mass-mass diagram
Each PK parameter identifies a curve in the mass-massdiagram.
1 line: a relation between the two masses.2 lines: the masses of the stars are determined
accordingly to the adopted gravity theory3 linesor more: gravity theories can be tested!
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The mass-mass diagram
The mass-mass diagram for the double pulsar contains:
- 5 curves from the measured PK parameters
- The mass ratio line (bonus!!!): orbit’s semimajor axis has been measured for both pulsars. Their ratio provides the system’s mass ratio, without calling into play any gravity theory!
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The mass-mass diagram
PSR A MASS (M)
PSR A MASS (M)Some10-4 M !
Confidence level: 2σ
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The Sardinia Radio Telescope
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The Sardinia Radio Telescope
Location: San Basilio (CA) - Loc. Pranu SanguniPosition: Lat. 39°29'50'' N - Long. 09°14'40'' E
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The Sardinia Radio Telescope
64 m single dish antenna
Active control of thesurface shape
Receivers in either primaryand Gregorian focus.
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The Sardinia Radio Telescope
The active surface allows:
- corrections due to wind and gravity deformations.
- surface control to perform very high frequency observations up to 100GHz.
- best performances for both primary focus and Gregorian focus observations.
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The Sardinia Radio Telescope
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Plans for SRT
• Northern Sky Survey for young pulsars and coalescing binaries.
• Timing of young pulsars, millisecond pulsars and coalescing binaries.
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Pulsar Timing Array
Pulsars discovered in Galactic Census also provide a networkof arms of a huge cosmic gravitational wave detector.
Perturbations in space-timecan be detected in pulsars’timing residuals.
PulsarPulsar TimingTiming ArrayArray
PTA:PTA:
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