GBT01A-075

Multifrequency Monitoring of a Massive Pulsar System

Abstract

The recently discovered young pulsar PSR J1740-3052 is in an eccentric 231-day orbit with a companion of at least 11 solar masses. The nature of the companion is still undetermined; though there is a late-type star coincident with the pulsar position, the magnitude of the advance of periastron in the pulsar timing solution and the small observed dispersion measure variations instead imply a more compact companion, probably an early B star, though we cannot completely rule out a black hole. Continued long-term timing and multifrequency polarimetric monitoring are essential to determine the nature of the companion and to study the interaction of the two stars. We propose to monitor PSR J1740-3052 at intervals of 2 weeks, observing at 1400 MHz, 2400 MHz, and either 600 MHz or 1040 MHz. In the 6 weeks prior to periastron, we ask for more frequent sampling (4-5 days) in order to obtain a clear picture of the dispersion measure variations.

**Investigators**
Name	Other *	Institution	Email	Phone
Ingrid Stairs	PI	NRAO - Green Bank	istairs@nrao.edu	(304)456-2213
Dick Manchester		Australia Telescope	rmanches@atnf.csiro.au	+61-2-9372-4313,+61 2 9372 4222
Andrew Lyne		NRAL	agl@jb.man.ac.uk	44-1477-571321 X 301

* PI = Principal Investigator; T = Thesis observations; S = Student

Front Ends

Prime Focus 1-3  6(0.51 to 0.69 GHz)
Prime Focus 2  A(0.91 to 1.23 GHz)
Gregorian L(1.15 to 1.73 GHz)
Gregorian S(1.73 to 2.6 GHz)

Back Ends

GBT Spectrometer
Spectral Processor
Berkley Caltech Pulsar Machine

Type of Observing

Point Source
Continuum
Monitor
Circular Polarization
Pulsar
High Time Resolution

Switching Type

Allocated time: 35.00 hours.

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