Conference

The Large Millimeter Telescope (LMT) is a 50m diameter telescope at an altitude of 4600 m in the country of Mexico. It is a joint project between the University of Massachusetts, Amherst and the Instituto Nacional de Astrofisica, Optica y Electronica (INAOE). At this time, the inner three rings of the telescope have been furnished with precision surface panels for an effective diameter of 32.5 m and effective surface rms better than 80 microns. With an active primary surface, the LMT can maintain this surface over a wide elevation range. While the outer rings will be procured and installed in the next 2 years, the telescope is into its third year of early science with two receivers, the Redshift Search Receiver (RSR) and AzTEC. I will provide a short description of the engineering and scientific status of the LMT. I will also summarize VLBI activities at the LMT to date, and present plans for a dual-polarization 1mm wavelength receiver for the LMT that will enable the telescope to participate in the EHT experiment by 2016.

The path from the current EHT to the full array capabilities has been mapped out over the past several years. Through the efforts of the EHT Technical Working Group and the full complement of experts involved in the project, we have a detailed plan and work breakdown to implement these improvements. I will describe the schedule for EHT expansion and enhancement from 2015 onward.

Convened in the summer of 2013, the EHT Technical Working Group (ETWG) was tasked with:1. Survey the capabilities at all EHT facilities 2. Establish a set of specifications for future EHT observations 3. Outline the technical developments needed to reach these goals 4. Based on prioritized science objectives, formulate a project roadmap that is grounded in technical feasibility with the resources available.This overview will report on the findings and conclusions arrived at by the ETWG and present specifications for future EHT observations at 230 and 345 GHz. I will also briefly discuss subsequent technical developments and the rollout of new equipment for the 2015 EHT observing campaign that will for the first time deploy recording at 16 Gb/s. With a relatively modest expansion over the next couple of years this mmVLBI system will be capable of 64 Gb/s for an aggregate bandwidth of 16 GHz i.e. 8x the bandwidth of existing EHT observations.

The supermassive black hole in the centre of the Milky Way, Sgr A*, is an ideal target for testing the properties of black holes. A number of experiments are being prepared or conducted, such as the monitoring of stellar orbits, the search for radio pulsars or the recording of an image of the shadow of a event horizon. The talk puts these efforts in context with other tests of general relativity and its alternatives. I will also compare the approaches in the Galactic centre, while concentrating in particular on the prospects of using pulsars as probes, also in combination with event horizon imaging.

In general relativity, astrophysical black holes are characterized uniquely in terms of their masses and spins and are described by the Kerr metric. The high sensitivity and resolution of the EHT will allow for unprecedented tests of the Kerr nature of black holes and, hence, of general relativity. I will present current and future limits on deviations from the Kerr metric from Sgr A* in the context of radiatively-inefficient accretion flow models. I will also show how largely model-independent constraints on such deviations can be obtained from the angular diameter of the photon ring of Sgr A* in combination with existing mass and distance measurements. Finally, I will describe a new general framework for the parametrization of deviations from the Kerr metric.

I will discuss the prospects for finding additional radio pulsars in the Galactic center region and their utility for probing general relativity and other constituents in the region. This will include discussions of neutron star populations; radio wave scattering in and toward the Galactic center; issues and progress in discovering pulsars; and the precision to which discoverable pulsars can be timed

GRAVITY is a new instrument combining the four 8m ESO Very Large Telescopes in Chile. Other than the BlackHoleCam / EHT with its focus on imaging the shadow of the black hole against the surrounding accretion flow, the goal of GRAVITY is to measure dynamical processes in the immediate vicinity of the black hole, for example the motion of matter close to the last stable orbit and relativistic effects in stellar orbits. Our presentation covers the experimental and astrophysical aspects of this project and highlights the complementarity with the submm interferometry to overcome the degeneracies in modelling the observations.