High Time Resolution Astrophysics in the Extremely Large Telescope Era : White Paper

Abstract

High Time Resolution Astrophysics (HTRA) concerns itself with observations on short scales normally defined as being lower than the conventional read-out time of a CCD. As such it is concerned with condensed objects such as neutron stars, black holes and white dwarfs, surfaces with extreme magnetic reconnection phenomena, as well as with planetary scale objects through transits and occultations. HTRA is the only way to make a major step forward in our understanding of several important astrophysical and physical processes; these include the extreme gravity conditions around neutron stars and stable orbits around stellar mass black holes. Transits, involving fast timing, can give vital information on the size of, and satellites around exoplanets. In the realm of fundamental physics very interesting applications lie in the regime of ultra-high time resolution, where quantum-physical phenomena, currently studied in laboratory physics, may be explored. From the short descriptions given below it can be seen that HTRA science covers the full gamut of observational optical/IR astronomy from asteroids to γ-rays bursts, contributing to four out six of AstroNet's fundamental challenges described in their Science Vision for European Astronomy. Giving the European-Extremely Large Telescope (E-ELT) an HTRA capability is therefore of paramount importance. We suggest that there are three possibilities for HTRA and E-ELT. These are, firstly giving the E-ELT first light engineering camera an HTRA science capability. Secondly, to include a small HTRA instrument within another instrument -Micado is a possibility here. Finally, to have separate fibre feeds from, say Optimos, to a dedicated HTRA instrument. In this case a small number of fibres (<10) could be positioned and would provide a flexible and low cost means to have an HTRA capability. By the time of E-ELT first light, there should be a number of significant developments in fast detectors, in particular in the infra-red (IR) region -already today small photon-counting IR arrays have been developed that should be mainstream technology in the next years.

Stochastic dark energy from inflationary quantum fluctuations

“…Note that this expression is derived as a leading order contri- Fig. 2), which is testable by the next generation of observatories such as Euclid [21] and ELT [22].…”

“…Still no statistically significant deviation of DE from an exact cosmological constant has been found 1 . The upcoming measurements of Large Synoptic Survey Telescope (LSST) [20], ESA's Euclid satellite mission [21] and the European Extreme Large Telescope (E-ELT) [22] will further constrain dynamical DE models. For example, the accuracy of Euclid [21] is projected to be a few percent for simple (1 or 2 parameter models) and weaker for more involved models.…”

VLT observations of the twoFermipulsars PSR J1357−6429 and PSR J1048−5832

“…In particular, five out of the seven γ-ray pulsars detected by NASA's Compton Gamma-ray Observatory (CGRO) satellite (see, e.g. Thompson 2008) have also been detected in the optical, suggesting that γ-ray detections indicate promising candidates for optical observations, since the emission at both energies seems to correlate with the strength of the magnetic field at the light cylinder (Shearer & Golden 2001;Shearer et al 2010). …”

The Galway astronomical Stokes polarimeter: an all-Stokes optical polarimeter with ultra-high time resolution

“…For GASP our main targets are isolated neutron stars, either pulsars or magnetars, and compact binary systems. Shearer et al (2010) give a review of the current state of optical polarimetric observations of these systems.…”

“…Optical observations and in particular polarimetric observations will be important to tie down the emission process. To date, no observations have been made of the optical polarisation from magnetars; see Shearer et al (2010) for a discussion of the possibilities.…”