Scientific objectives of the Hot Universe Baryon Surveyor (HUBS) mission

Bregman, Joel; Cen, Renyue; Chen, Yang; Cui, Wei; Fang, Taotao; Guo, Fulai; Hodges-Kluck, Edmund; Huang, Rui; Ho, Luis C.; Ji, Li; Ji, Suoqing; Kang, Xi; Lai, Xiaoyu; Li, Hui; Li, Jiangtao; Li, Miao; Li, Xiangdong; Li, Yuan; Li, Zhaosheng; Liang, Guiyun; Liu, Helei; Liu, Wenhao; Lu, Fangjun; Mao, Junjie; Ponti, Gabriele; Qu, Zhijie; Shan, Chenxi; Shao, Lijing; Shi, Fangzheng; Shu, Xinwen; Sun, Lei; Sun, Mouyuan; Tong, Hao; Wang, Junfeng; Wang, Junxian; Wang, Q. Daniel; Wang, Song; Wang, Tinggui; Wang, Weiyang; Wang, Zhongxiang; Xu, Dandan; Xu, Haiguang; Xu, Heng; Xu, Renxin; Xu, Xiaojie; Xue, Yongquan; Yang, Hang; Yuan, Feng; Zhang, Shuinai; Zhang, Yuning; Zhang, Zhongli; Zhao, Yuanyuan; Zhou, Enping; Zhou, Ping

doi:10.1007/s11433-023-2149-y

Cited by 12 publications

(5 citation statements)

References 430 publications

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“…This possibility is suggestively consistent with present binary population studies, in which high-mass X-ray binaries are more numerous in low-metallicity galaxies [59,60]. It is required future follow-up investigations with larger sample of SNRs using a microcalorimeter onboard XRISM [24] and forthcoming missions such as Athena [25], Lynx [26], LEM [27], and HUBS [28].…”

Section: Pos(multif2023)044supporting

confidence: 70%

“…Progenitor constraint using line ratios of the CNO elements in supernova remnants Hiroyuki Uchida microcalorimeter observations with XRISM [24] launched in 2023 and future missions such as Athena [25], Lynx [26], LEM [27], and HUBS [28]. We thus demonstrate our calculation and method in this paper for near future high-energy-resolution X-ray observations of SNRs.…”

Section: Pos(multif2023)044mentioning

confidence: 65%

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Progenitor constraint using line ratios of the CNO elements in supernova remnants

Uchida,

Narita

2024

Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources XIV — PoS(MULTIF2023)

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Investigating the nature of progenitors is crucial for understanding the origin and mechanism of core-collapse and thermonuclear supernovae (SNe). While several methods have been developed to derive progenitor properties so far, many questions remain poorly understood. In this paper we demonstrate an observational approach to constrain progenitors of supernova remnants (SNRs) using abundances of carbon (C), nitrogen (N), and oxygen (O) in shock-heated circumstellar material (CSM). Our calculations with stellar evolution codes indicate that a total amount of these CNO elements will provide a more sensitive determination of the progenitor masses than the conventional method based on ejecta abundances. If the CNO lines (particularly those of C and N) are detected and measured their abundance ratios accurately, they can provide relatively robust constraint on the progenitor mass (and in some cases the rotation velocity) of SNRs. Since our method requires a better energy resolution and larger effective area in the soft X-ray band (< 1 keV), XRISM launched on September 7, 2023 and next-generation microcalorimeter missions such as Athena, Lynx, LEM, and HUBS will be adequate and will bring a new insight into link between the progenitors and their remnants.

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Section: Pos(multif2023)044supporting

confidence: 70%

Section: Pos(multif2023)044mentioning

confidence: 65%

Progenitor constraint using line ratios of the CNO elements in supernova remnants

Uchida,

Narita

2024

Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources XIV — PoS(MULTIF2023)

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“…In future work, it is desirable to study a larger sample of observed galaxies in nearby clusters, such as those afforded by Chandra and the ongoing eROSITA all-sky survey, to better probe the effect of RPS and other environmental effects on the star formation and global gas content of cluster galaxies, which in turn would be useful for calibrating next-generation cosmological simulations. Future missions with the potential to provide accurate abundance measurements for the hot gas corona, e.g., the recently launched XRISM (Tashiro 2022) and the planned HUBS (Bregman et al 2023) and Line Emission Mapper (Kraft et al 2022), would promise to shed light on the difference between accreted IGM and internally supplied hot gas.…”

Section: Discussionmentioning

confidence: 99%

X-Ray Constraints on the Hot Gaseous Corona of Edge-on Late-type Galaxies in Virgo

Hou,

He,

et al. 2024

ApJ

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We present a systematic study of the putative hot gas corona around late-type galaxies (LTGs) residing in the Virgo cluster, based on archival Chandra observations. Our sample consists of 21 nearly edge-on galaxies representing a range of star formation rate (SFR) of 0.2–3 M ⊙ yr−1 and a range of stellar mass (M *) of (0.2–10) × 1010 M ⊙, the majority of which have not been explored with high-sensitivity X-ray observations so far. Significant extraplanar diffuse X-ray (0.5–2 keV) emission is detected in only three LTGs, which are also the three galaxies with the highest SFR. A stacking analysis is performed for the remaining galaxies without individual detection, dividing the whole sample into two subsets based on SFR, stellar mass, or specific SFR. Only the high-SFR bin yields a significant detection, which has a value of L X ∼ 3 × 1038 erg s−1 per galaxy. The stacked extraplanar X-ray signals of the Virgo LTGs are consistent with the empirical L X–SFR and L X–M * relations found among highly inclined disk galaxies in the field, but appear to be systematically lower than those of a comparison sample of simulated star-forming galaxies in clusters identified from the Illustris-TNG100 simulation. The apparent paucity of hot gas coronae in the sampled Virgo LTGs might be understood as the net outcome of the long-lasting effect of ram pressure stripping exerted by the hot intracluster medium and in-disk star-forming activity acting on shorter timescales. A better understanding of the roles of environmental effects in regulating the hot gas content of cluster galaxies invites sensitive X-ray observations for a large sample of galaxies.

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“…Current low-spectral-resolution observations cannot provide strong constraints on these scenarios, especially the first two possibilities. Instead, better constraints on the temperature distribution and abundance variation are expected to be obtained by future missions such as Athena, Hot Universe Baryon Surveyor, and the Line Emission Mapper (Nandra et al 2013;Cui et al 2020;Kraft et al 2022;Bregman et al 2023).…”

Section: Comparison Between O87 and Feo Ratiosmentioning

confidence: 99%

The XMM-Newton Line Emission Analysis Program (X-LEAP). II. The Multiscale Temperature Structures in the Milky Way Hot Gas

Qu,

Pan,

Bregman

et al. 2024

ApJ

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This paper presents the multiscale temperature structures in the Milky Way (MW) hot gas, as part of the XMM-Newton Line Emission Analysis Program, surveying the O vii, O viii, and Fe-L band emission features in the XMM-Newton archive. In particular, we define two temperature tracers, I OVIII/I OVII (O87) and I FeL/(I OVII + I OVIII) (FeO). These two ratios cannot be explained simultaneously using single-temperature collisional ionization models, which indicates the need for multitemperature structures in hot gas. In addition, we show three large-scale features in the hot gas: the eROSITA bubbles around the Galactic center (GC), the disk, and the halo. In the eROSITA bubbles, the observed line ratios can be explained by a log-normal temperature distribution with a median of log T / K ≈ 6.4 and a scatter of σ T ≈ 0.2 dex. Beyond the bubbles, the line ratio dependence on the Galactic latitude suggests higher temperatures around the midplane of the MW disk. The scale height of the temperature variation is estimated to be ≈2 kpc assuming an average distance of 5 kpc for the hot gas. The halo component is characterized by the dependence on the distance to the GC, showing a temperature decline from log T / K ≈ 6.3 to 5.8. Furthermore, we extract the autocorrelation and cross-correlation functions to investigate the small-scale structures. O87 and FeO ratios show a consistent autocorrelation scale of ≈5° (i.e., ≈400 pc at 5 kpc), which is consistent with the expected physical sizes of X-ray bubbles associated with star-forming regions or supernova remnants. Finally, we examine the cross-correlation between the hot and UV-detected warm gas and show an intriguing anticorrelation.

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Scientific objectives of the Hot Universe Baryon Surveyor (HUBS) mission

Cited by 12 publications

References 430 publications

Progenitor constraint using line ratios of the CNO elements in supernova remnants

Progenitor constraint using line ratios of the CNO elements in supernova remnants

X-Ray Constraints on the Hot Gaseous Corona of Edge-on Late-type Galaxies in Virgo

The XMM-Newton Line Emission Analysis Program (X-LEAP). II. The Multiscale Temperature Structures in the Milky Way Hot Gas

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