X-Ray, Optical, and Near-infrared Monitoring of the New X-Ray Transient MAXI J1820+070 in the Low/Hard State

被引：14

作者：

Shidatsu, Megumi ^{[1
]}

Nakahira, Satoshi ^{[2
]}

Yamada, Satoshi ^{[3
]}

Kawamuro, Taiki ^{[4
]}

Ueda, Yoshihiro ^{[3
]}

Negoro, Hitoshi ^{[5
]}

Murata, Katsuhiro L. ^{[6
]}

Itoh, Ryosuke ^{[6
]}

Tachibana, Yutaro ^{[6
]}

Adachi, Ryo ^{[6
]}

Yatsu, Yoichi ^{[6
]}

Kawai, Nobuyuki ^{[7
]}

Hanayama, Hidekazu ^{[7
]}

Horiuchi, Takashi ^{[7
]}

Akitaya, Hiroshi ^{[8
]}

Saito, Tomoki ^{[9
]}

Takayama, Masaki ^{[9
]}

Ohshima, Tomohito ^{[9
]}

Katoh, Noriyuki ^{[9
]}

Takahashi, Jun ^{[9
]}

Nagayama, Takahiro ^{[10
]}

Yamanaka, Masayuki ^{[11
]}

Kawabata, Miho ^{[12
]}

Nakaoka, Tatsuya ^{[12
]}

Takagi, Seiko ^{[13
]}

Morokuma, Tomoki ^{[14
]}

Morihana, Kumiko ^{[15
]}

Maehara, Hiroyuki ^{[16
]}

Sekiguchi, Kazuhiro ^{[17
]}

机构：

[1] Ehime Univ, Dept Phys, 2-5 Bunkyocho, Matsuyama, Ehime 7908577, Japan

[2] RIKEN, High Energy Astrophys Lab, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[3] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto, Kyoto 6068502, Japan

[4] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[5] Nihon Univ, Dept Phys, Chiyoda Ku, 1-8-14 Kanda Surugadai, Tokyo 1018308, Japan

[6] Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan

[7] Natl Inst Nat Sci, Natl Astron Observ Japan, Ishigakijima Astron Observ, 1024-1 Arakawa, Ishigaki, Okinawa 9070024, Japan

[8] Saitama Univ, Grad Sch Sci & Engn, Sakura Ku, Simo Okubo 135, Saitama 3388570, Japan

[9] Univ Hyogo, Ctr Astron, Nishiharima Astron Observ, 407-2 Nishigaichi, Sayo, Hyogo 6795313, Japan

[10] Kagoshima Univ, Grad Sch Sci & Engn, 1-21-35 Korimoto, Kagoshima 8900065, Japan

[11] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan

[12] Hiroshima Univ, Dept Phys Sci, Kagamiyama 1-3-1, Higashihiroshima 7398526, Japan

[13] Hokkaido Univ, Dept Cosmosci, Kita Ku, Kita 10 Nishi 8, Sapporo, Hokkaido 0600810, Japan

[14] Univ Tokyo, Grad Sch Sci, Inst Astron, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan

[15] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan

[16] Kyoto Univ, Grad Sch Sci, Okayama Observ, 3037-5 Honjo, Asakuchi, Okayama 7190232, Japan

[17] Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

来源：

ASTROPHYSICAL JOURNAL | 2018年 / 868卷 / 01期

关键词：

accretion; accretion disks; black hole physics; X-rays: binaries; X-rays: individual (MAXI J1820+070); BLACK-HOLE CANDIDATE; RADIO-EMISSION; COMPACT JET; ACCRETION; BINARIES; MASS; MITSUME; DISC; ABSORPTION; TELESCOPES;

D O I：

10.3847/1538-4357/aae929

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report X-ray, optical, and near-infrared monitoring of the new X-ray transient MAXI J1820+070 discovered with MAXI on 2018 March 11. Its X-ray intensity reached similar to 2 crab at 2-20 keV at the end of March, and then gradually decreased until the middle of June. In this period, the X-ray spectrum was described by Comptonization of the disk emission, with a photon index of similar to 1.5 and an electron temperature of similar to 50 keV, which is consistent with a black hole X-ray binary in the low/hard state. The electron temperature was slightly decreased, and the photon index increased, with increasing flux. The source showed significant X-ray flux variation on a timescale of seconds. This short-term variation was found to be associated with changes in the spectral shape, and the photon index became slightly harder at higher fluxes. This suggests that the variation was produced by a change in the properties of the hot electron cloud responsible for the strong Comptonization. Modeling a multi-wavelength spectral energy distribution around the X-ray flux peak at the end of March, covering the near-infrared to X-ray bands, we found that the optical and near-infrared fluxes were likely contributed substantially by the jet emission. Before this outburst, the source was never detected in the X-ray band with MAXI (with a 3 sigma upper limit of similar to 0.2 mcrab at 4-10 keV, obtained from seven years of data from 2009 to 2016), whereas weak optical and infrared activity was found at flux levels similar to 3 orders of magnitude lower than the peak fluxes in the outburst.

引用

页数：11

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