Super DIOS: Future X-ray Spectroscopic Mission to Search for Dark Baryons

Yamada, S.; Ohashi, T.; Ishisaki, Yoshitaka; Ezoe, Yuichiro; Ichinohe, Yuto; Kitazawa, Shun; Kosaka, Koji; Hayakawa, Ritsuko; Nunomura, K.; Mitsuda, Kazuhisa; Yamasaki, Noriko Y.; Kikuchi, T.; Hayashi, T.; Muramatsu, H.; Nakashima, Yoshiki; Tawara, Yuzuru; Mitsuishi, Ikuyuki; Babazaki, Yasunori; Seki, Daikichi; Otsuka, Kentaro; Ishihara, Makoto; Osato, Ken; Ota, Naomi; Tomariguchi, M.; Nagai, Daisuke; Lau, Erwin T.; Sato, Kousuke

doi:10.1007/s10909-018-1918-z

Cited by 8 publications

(3 citation statements)

References 17 publications

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“…The most direct effect is the significantly higher FoM than CCD X‐ray missions (Table ). In particular, also with their large FOVs, HUBS and Super‐DIOS will be the most efficient instruments in detecting the extended hot CGM around local galaxies, although as small missions their effective areas are not superb (Cui et al ; Yamada et al ). Angular resolution is not as important as in the study of point‐like sources, because point source contributions (stellar sources, AGN) can always be well removed in spectral space, especially in a narrow band.…”

Section: What Can We Do In the Future?mentioning

confidence: 99%

An X‐ray view of the hot circum‐galactic medium

2020

Astron Nachr

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The hot circum‐galactic medium (CGM) represents the hot gas distributed beyond the stellar content of the galaxies while typically within their dark matter halos. It serves as a depository of energy and metal‐enriched materials from galactic feedback and a reservoir from which the galaxy acquires fuels to form stars. It thus plays a critical role in the coevolution of galaxies and their environments. X‐rays are one of the best ways to trace the hot CGM. I will briefly review what we have learned about the hot CGM based on X‐ray observations over the past two decades, and what we still do not know. I will also briefly prospect what may be the foreseeable breakthrough in the next one or two decades with future X‐ray missions.

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Section: What Can We Do In the Future?mentioning

confidence: 99%

An X‐ray view of the hot circum‐galactic medium

2020

Astron Nachr

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“…The most direct effect is the significantly higher than CCD X-ray missions (Table 2 ). In particular, also with their large FOVs, HUBS and Super-DIOS will be the most efficient instruments in detecting the extended hot CGM around local galaxies, although as small missions, their effective areas are not superb (Cui et al, 2019;Yamada et al, 2018). Angular resolution is not as important as in the study of point-like sources, because point source contributions (stellar sources, AGN) can always be well removed in spectral space, especially in narrow-band.…”

Section: Future Focusing X-ray Telescopesmentioning

confidence: 99%

An X-ray View of the Hot Circum-Galactic Medium

2020

Preprint

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The hot circum-galactic medium (CGM) represents the hot gas distributed beyond the stellar content of the galaxies while typically within their dark matter halos. It serves as a depository of energy and metal-enriched materials from galactic feedback and a reservoir from which the galaxy acquires fuels to form stars. It thus plays a critical role in the coevolution of galaxies and their environments. X-rays are one of the best ways to trace the hot CGM. I will briefly review what we have learned about the hot CGM based on X-ray observations over the past two decades, and what we still do not know. I will also briefly prospect what may be the foreseeable breakthrough in the next one or two decades with future X-ray missions.

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“…These measurements will be crucial to detect and "map" the bulk of the ordinary matter in our nearby Universe. The yet to be approved Japanese SuperDIOS mission (Yamada et al, 2018) will extend the capabilities of HUBS. Its 10 arcsec spatial resolution will allow a robust filtering of contaminating X-ray point sources and thus a more reliable census of diffuse warm-hot baryons.…”

Section: Future Studies Of Hot Atmospheresmentioning

confidence: 99%

Hot atmospheres of galaxies, groups, and clusters of galaxies

Werner,

Mernier

2020

Preprint

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Most of the ordinary matter in the local Universe has not been converted into stars but resides in a largely unexplored diffuse, hot, X-ray emitting plasma. It pervades the gravitational potentials of massive galaxies, groups and clusters of galaxies, as well as the filaments of the cosmic web. The physics of this hot medium, such as its dynamics, thermodynamics and chemical composition can be studied using X-ray spectroscopy in great detail. Here, we present an overview of the basic properties and discuss the self similarity of the hot "atmospheres" permeating the gravitational halos from the scale of galaxies, through groups, to massive clusters. Hot atmospheres are stabilised by the activity of supermassive black holes and, in many ways, they are of key importance for the evolution of their host galaxies. The hot plasma has been significantly enriched in heavy elements by supernovae during the period of maximum star formation activity, probably more than 10 billion years ago. High resolution X-ray spectroscopy just started to be able to probe the dynamics of atmospheric gas and future space observatories will determine the properties of the currently unseen hot diffuse medium throughout the cosmic web.

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Super DIOS: Future X-ray Spectroscopic Mission to Search for Dark Baryons

Cited by 8 publications

References 17 publications

An X‐ray view of the hot circum‐galactic medium

An X‐ray view of the hot circum‐galactic medium

An X-ray View of the Hot Circum-Galactic Medium

Hot atmospheres of galaxies, groups, and clusters of galaxies

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