TY - JOUR
T1 - Amount of intergalactic dust
T2 - Constraints from distant supernovae and the thermal history of the intergalactic medium
AU - Inoue, Akio K.
AU - Kamaya, Hideyuki
N1 - Copyright:
Copyright 2008 Elsevier B.V., All rights reserved.
PY - 2004/5/11
Y1 - 2004/5/11
N2 - In this paper we examine the allowed amount of intergalactic (IG) dust, which is constrained by extinction and reddening of distant Type Ia supernovae (SNe Ia) and the thermal history of the intergalactic medium (IGM) affected by dust photoelectric heating. Based on the observational cosmic star formation history, we find an upper bound of χ, the mass ratio of the IG dust to the total metal in the Universe, as χ ≲ 0.1 for 10 Å ≲ a ≲ 0.1 μm and χ ≲ 0.1(a/0.1 μm) for 0.1 ≲ a ≲ 1 μm, where a is a characteristic grain size of the IG dust. This upper bound of χ ∼ 0.1 suggests that the dust-to-metal ratio in the IGM is smaller than the current Galactic value. The corresponding allowed density of the IG dust increases from ∼10-34 g cm-3 at z = 0 to ∼10 -33 g cm-3 at z ∼ 1, and keeps almost the value toward higher redshift. This causes IG extinction of ≲0.2 mag at the observer's B band for z ∼ 1 sources and that of ≲1 mag for higher redshift sources. Furthermore, if E(B-V) ∼ 0.1 mag at the observer's frame against z ≳ 1 sources is detected, we can conclude that a typical size of the IG dust is ≲ 100 Å. The signature of the 2175-Å feature of small graphite may be found as a local minimum at z ∼ 2.5 in a plot of the observed E(B-V) as a function of the source redshift. Finally, the IGM mean temperature at z ≲ 1 can be still higher than 104 K, provided the size of the IG dust is ≲100 Å.
AB - In this paper we examine the allowed amount of intergalactic (IG) dust, which is constrained by extinction and reddening of distant Type Ia supernovae (SNe Ia) and the thermal history of the intergalactic medium (IGM) affected by dust photoelectric heating. Based on the observational cosmic star formation history, we find an upper bound of χ, the mass ratio of the IG dust to the total metal in the Universe, as χ ≲ 0.1 for 10 Å ≲ a ≲ 0.1 μm and χ ≲ 0.1(a/0.1 μm) for 0.1 ≲ a ≲ 1 μm, where a is a characteristic grain size of the IG dust. This upper bound of χ ∼ 0.1 suggests that the dust-to-metal ratio in the IGM is smaller than the current Galactic value. The corresponding allowed density of the IG dust increases from ∼10-34 g cm-3 at z = 0 to ∼10 -33 g cm-3 at z ∼ 1, and keeps almost the value toward higher redshift. This causes IG extinction of ≲0.2 mag at the observer's B band for z ∼ 1 sources and that of ≲1 mag for higher redshift sources. Furthermore, if E(B-V) ∼ 0.1 mag at the observer's frame against z ≳ 1 sources is detected, we can conclude that a typical size of the IG dust is ≲ 100 Å. The signature of the 2175-Å feature of small graphite may be found as a local minimum at z ∼ 2.5 in a plot of the observed E(B-V) as a function of the source redshift. Finally, the IGM mean temperature at z ≲ 1 can be still higher than 104 K, provided the size of the IG dust is ≲100 Å.
KW - Cosmology: theory
KW - Dust, extinction
KW - Intergalactic medium
KW - Quasars: absorption lines
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U2 - 10.1111/j.1365-2966.2004.07686.x
DO - 10.1111/j.1365-2966.2004.07686.x
M3 - Article
AN - SCOPUS:2542533902
VL - 350
SP - 729
EP - 744
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -