Erratum: “The Lyman-alpha Solar Telescope (LST) for the ASO-S mission — I. Scientific objectives and overview” (2019, RAA, 19, 158)

The Advanced Space-based Solar Observatory (ASO-S) is a mission proposed for the 25th solar maximum by the Chinese solar community. The scientific objectives are to study the relationships between the solar magnetic field, solar flares and coronal mass ejections (CMEs). Three payloads are deployed: the Full-disk vector MagnetoGraph (FMG), the Lyman-α Solar Telescope (LST) and the Hard X-ray Imager (HXI). ASO-S will perform the first simultaneous observations of the photospheric vector magnetic field, non-thermal imaging of solar flares, and the initiation and early propagation of CMEs on a single platform. ASO-S is scheduled to be launched into a 720 km Sun-synchronous orbit in 2022. This paper presents an overview of the mission till the end of Phase-B and the beginning of Phase-C.

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“…Figure 2 displays the optical and mechanical layouts of LST. For details on LST, we refer readers to Chen et al (2019) and Li et al (2019b).…”

Section: Payload Deploymentmentioning

confidence: 99%

Advanced Space-based Solar Observatory (ASO-S): an overview

Gan

Zhu

Deng

et al. 2019

Res. Astron. Astrophys.

132

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“…So, when the LST/SDI and LST/WST observe in fast mode, by default, only a partial image of 1024 × 1024 pixels will be recorded in order to reduce the data volume onboard. For details on the observing mode, we refer readers to Li et al (2019).…”

Section: Observation Modes and Data Volumementioning

confidence: 99%

The Science Operations and Data Center (SODC) of the ASO-S mission

Gan

et al. 2019

Res. Astron. Astrophys.

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A ground data analysis center is very important to the success of a mission. We introduce the Science Operations and Data Center (SODC) for the ASO-Smission, which consists of a scientific operation subcenter, a data management subcenter, a data analysis subcenter and a user service subcenter. Themission planning process, instrument observation modes and the data volume are presented. We describe the data flow and processing procedures from spacecraft telemetry to high-level science data, and the long-term archival as well. The data policy and distributions are also briefly introduced.

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“…LST will observe all areas from the solar disk to the inner corona up to 2.5 R ⊙ in the Lyα line, and the coronal polarization images in 700.0 nm waveband, along with the solar disk image in 360.0 nm waveband. The scientific objectives are summarized below, and please refer to Gan et al (2019), Li et al (2019) and Feng et al (2019a) for details.…”

Section: Introductionmentioning

confidence: 99%

“…The scientific objectives and overview have been presented in Li et al (2019) (Paper I) and the data products and diagnostics have been presented in Feng et al (2019a) (Paper III). In this paper (Paper II), we describe the detailed design of the LST instruments in Section 2, including optical design, stray-light suppression, mechanical structure, thermal control and electronics.…”

Section: Introductionmentioning

confidence: 99%

The Lyman-alpha Solar Telescope (LST) for the ASO-S mission – II. design of LST

Chen¹,

Li²,

Song³

et al. 2019

Res. Astron. Astrophys.

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As one of the three payloads for the Advanced Space-based Solar Observatory (ASO-S) mission, the Lyman-alpha (Lyα) Solar Telescope (LST) is composed of three instruments: a Solar Corona Imager (SCI), a Lyα Solar Disk Imager (SDI) and a full-disk White-light Solar Telescope (WST). When working in-orbit, LST will simultaneously perform high-resolution imaging observations of all regions from the solar disk to the inner corona up to 2.5 R⊙ (R⊙ stands for the mean solar radius) with a spatial resolution of 4.8″ and 1.2″ for coronal and disk observations, respectively, and a temporal resolution of 30 – 120 s and 1 – 120 s for coronal and disk observations, respectively. The maximum exposure time can be up to 20 s due to precise pointing and image stabilization function. Among the three telescopes of LST, SCI is a dual-waveband coronagraph simultaneously and independently observing the inner corona in the HI Lyα (121.6±10 nm) line and white light (WL) (700±40 nm) wavebands by using a narrowband Lyα beam splitter and has a field of view (FOV) from 1.1 to 2.5 R⊙. The stray-light suppression level can attain <10−6 B⊙ (B⊙ is the mean brightness of the solar disk) at 1.1 R⊙ and ≤5×10−8 B⊙ at 2.5 R⊙. SDI and WST are solar disk imagers working in the Lyα line and 360.0 nm wavebands, respectively, which adopt an off-axis two-mirror reflective structure with an FOV up to 1.2 R⊙, covering the inner coronal edge area and relating to coronal imaging. We present the up-to-date design for the LST payload.

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Erratum: “The Lyman-alpha Solar Telescope (LST) for the ASO-S mission — I. Scientific objectives and overview” (2019, RAA, 19, 158)

Abstract: there is an error occurred in Table 2 about the image size of SCI UV in the 'Event' mode: the image size 4608×4608 should be replaced by 2048×2048. This correction is indicated in bold face in the following table.

Cited by 8 publications

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Advanced Space-based Solar Observatory (ASO-S): an overview

Advanced Space-based Solar Observatory (ASO-S): an overview

The Science Operations and Data Center (SODC) of the ASO-S mission

The Lyman-alpha Solar Telescope (LST) for the ASO-S mission – II. design of LST

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