The KaVA and KVN Pulsar Project

TL;DR

This paper explores the use of the combined KaVA array for high-frequency pulsar observations, aiming to discover and monitor pulsars, especially near the Galactic Center, where high-frequency data is crucial.

Contribution

It introduces the application of the KaVA array for high-frequency pulsar observations and discusses its potential for discovering pulsars in challenging regions.

Findings

Initial test observations of known pulsars with KVN.

Potential for high-frequency pulsar searches near the Galactic Center.

Advantages of KaVA for pulsar astronomy at 22 GHz.

Abstract

We present our work towards using the Korean VLBI (Very Long Baseline Interferometer) Network (KVN) and VLBI Exploration of Radio Astronomy (VERA) arrays combined into the KVN and VERA Array (KaVA) for observations of radio pulsars at high frequencies ($\simeq$22-GHz). Pulsar astronomy is generally focused at frequencies approximately 0.3 to several GHz and pulsars are usually discovered and monitored with large, single-dish, radio telescopes. For most pulsars, reduced radio flux is expected at high frequencies due to their steep spectrum, but there are exceptions where high frequency observations can be useful. Moreover, some pulsars are observable at high frequencies only, such as those close to the Galactic Center. The discoveries of a radio-bright magnetar and a few dozen extended Chandra sources within 15 arc-minute of the Galactic Center provide strong motivations to make use of the KaVA frequency band for searching pulsars in this region. Here, we describe the science targets and report progresses made from the KVN test observations for known pulsars. We then discuss why KaVA pulsar observations are compelling.