Detection capabilities of the Athena X-IFU for the warm-hot intergalactic medium using gamma-ray burst X-ray afterglows

被引：8

作者：

Walsh, Sarah ^{[1
]}

McBreen, Sheila ^{[1
]}

Martin-Carrillo, Antonio ^{[1
]}

Dauser, Thomas ^{[2
,3
]}

Wijers, Nastasha ^{[4
]}

Wilms, Joern ^{[2
,3
]}

Schaye, Joop ^{[4
]}

Barret, Didier ^{[5
]}

机构：

[1] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland

[2] Univ Erlangen Nurnberg, Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany

[3] Univ Erlangen Nurnberg, ECAP, Sternwartstr 7, D-96049 Bamberg, Germany

[4] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[5] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 642卷

关键词：

gamma-ray burst: general; large-scale structure of Universe; X-rays: general; intergalactic medium; instrumentation: detectors; LINE-OF-SIGHT; XMM-NEWTON; EAGLE SIMULATIONS; COMPLETE SAMPLE; LIGHT CURVES; ABSORPTION; BARYONS; CHANDRA; FOREST; WHIM;

D O I：

10.1051/0004-6361/202037775

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

At low redshifts, the observed baryonic density falls far short of the total number of baryons predicted. Cosmological simulations suggest that these baryons reside in filamentary gas structures, known as the warm-hot intergalactic medium (WHIM). As a result of the high temperatures of these filaments, the matter is highly ionised such that it absorbs and emits far-UV and soft X-ray photons. Athena, the proposed European Space Agency X-ray observatory, aims to detect the "missing" baryons in the WHIM up to redshifts of z = 1 through absorption in active galactic nuclei and gamma-ray burst (GRB) afterglow spectra, allowing for the study of the evolution of these large-scale structures of the Universe. This work simulates WHIM filaments in the spectra of GRB X-ray afterglows with Athena using the SImulation of X-ray TElescopes framework. We investigate the feasibility of their detection with the X-IFU instrument, through OVII (E = 573 eV) and OVIII (E = 674 eV) absorption features, for a range of equivalent widths imprinted onto GRB afterglow spectra of observed starting fluxes ranging between 10(-12) and 10(-10) erg cm(-2) s(-1), in the 0.3-10 keV energy band. The analyses of X-IFU spectra by blind line search show that Athena will be able to detect OVII-OVIII absorption pairs with EWOVII > 0.13 eV and EWOVIII > 0.09 eV for afterglows with F > 2 x 10(-11) erg cm(-2) s(-1). This allows for the detection of approximate to 45-137 OVII-OVIII absorbers during the four-year mission lifetime. The work shows that to obtain an OVII-OVIII detection of high statistical significance, the local hydrogen column density should be limited at N-H < 8 x 10(20) cm(-2).

引用

页数：13

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