Development of Solid-State Photomultiplier-Based Infrared Photometers and High Time-Resolution Observations of Young Pulsars

Details Development of Solid-State Photomultiplier-Based Infrared Photometers and High Time-Resolution Observations of Young Pulsars Development of Solid-State Photomultiplier-Based Infrared Photometers and High Time-Resolution Observations of Young Pulsars

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997phdt.........2e&link_type=abstract

Thesis (PHD). HARVARD UNIVERSITY , Source DAI-B 58/05, p. 2469, Nov 1997, 197 pages.

Computer Science

Performance

2

Crab Nebula Pulsar, Large Magellanic Cloud Pulsar

Scientific paper

We present infrared to γ-ray studies of the pulsar emission mechanism, based on two young pulsars, the Crab Nebula pulsar and 0540-69, and novel infrared instrumentation and advanced Fourier techniques used to study them. We discuss the design, construction, and performance of two high-speed near-infrared photometers using Solid-State Photomultiplier detectors. These instruments provide photon-counting capability and sub-microsecond time response, both never before achieved in the infrared waveband. We then present high signal-to-noise observations of the Crab Nebula pulsar using the first of these instruments on the Multiple Mirror Telescope. We present the pulse profiles over the infrared to ultraviolet wavelength range, and we analyze the pulse shape as a function of wavelength. We also create both phase-averaged and phase-resolved color spectra of the pulsar emission. We find many trends in the pulse shape versus wavelength and spectral evolution versus phase, several of which were previously unknown and are not predicted by current pulsar emission models. We extend our analysis to higher energies, including γ-ray and X-ray pulse profiles. Comparing these profiles to the IR-UV profiles, we find that many of the trends continue over ~7 decades in energy. We also find interesting new evidence of a turnover in many trends near energies ~1 eV, and a previously unknown reversal in the shape of Peak 2. Next we present a summary of useful Fourier techniques for pulsar time series analysis. The topics we cover include larger-than-core-memory Fourier transforms, the response of DFTs to signals with integral and non-integral frequencies, techniques for response correction for non-integral frequencies, the response of DFTs to signals with frequency derivatives, and novel techniques to correct the Fourier response and measure the frequency derivatives. Finally, we present a ROSAT X-ray timing study of the Large Magellanic Cloud pulsar 0540-69, using archival observations. We discuss the ROSAT observations and the data reduction techniques used to determine the pulsar's local frequency. Next, we present the pulsar timing solution as determined by these measurements. We move on to a refined solution using pulse time-of-arrival analyses. Finally, we discuss the implications of these results for understanding the timing behavior of 0540-69.

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