The ASTRO-H (Hitomi) x-ray astronomy satellite

Abstract

The Hitomi (ASTRO-H) mission is the sixth Japanese X-ray astronomy satellite developed by a large international collaboration, including Japan, USA, Canada, and Europe. The mission aimed to provide the highest energy resolution ever achieved at E > 2 keV, using a microcalorimeter instrument, and to cover a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. After a successful launch on 2016 February 17, the spacecraft lost its function on 2016 March 26, but the commissioning phase for about a month provided valuable information on the on-board instruments and the spacecraft

Exploring the spectral variability of the Seyfert 1.5 galaxy Markarian 530 with Suzaku

“…The scenario is consistent with observations of other sources like NGC 5506, an intermediate Seyfert with a complex Fe region (Bianchi & Matt 2002), and Mrk 279, a Seyfert 1 with ionised lines likely originating from the tours (Costantini et al 2010). A future mission like XARM, with Hitomi-like (Takahashi et al 2016) spectral resolution will advance this work.…”

MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

“…Future work will be needed to understand such selection biases and categorise individual protoclusters with, e.g., X-ray properties (Gobat et al 2011;Valentino et al 2016;Wang et al 2016) and Hi tomography (Lee et al 2016). The upcoming eROSITA (Merloni et al 2012), a successor to the ASTRO-H (Hitomi, Takahashi et al 2016), and the Prime Focus Spectrograph on the Subaru Telescope (Tamura et al 2016) will possess the exceptional capability needed to reveal these unique objects.…”

The FABLE simulations: a feedback model for galaxies, groups, and clusters

“…In X-rays, the upcoming eROSITA telescope (Merloni et al 2012;Pillepich et al 2012) is expected to detect as many as one hundred thousand groups and clusters of galaxies out to z ∼ 1 while observations of the Sunyaev-Zel'dovich effect (SZ) with SPT-3G (Benson et al 2014) and ACTpol (Henderson et al 2016) extend the search to higher redshift. Detailed follow-up observations will be possible at X-ray wavelengths with missions such as XARM (replacement for Hitomi; Takahashi et al 2010Takahashi et al , 2016 and Athena (Nandra et al 2013) and at optical and near-infrared wavelengths with ground-based surveys E-mail: n.henden@ast.cam.ac.uk such as the Dark Energy Survey (Dark Energy Survey Collaboration 2005) and the Large Synoptic Survey Telescope (LSST Dark Energy Science Collaboration 2012), as well as future space-based missions such as Euclid (Laureijs et al 2011).…”