2017年IOAA理论第10题-GOTO望远镜 - 版本历史

2022年7月30日 (六) 22:15 Caroldong

2022-07-30T22:15:57Z

2022年7月30日 (六) 21:14 Caroldong

2022-07-30T21:14:18Z

2022年7月30日 (六) 20:46 Caroldong

2022-07-30T20:46:54Z

Caroldong：/* 英文原题 */

2019-10-10T20:21:21Z

‎英文原题

2019年10月10日 (四) 20:17 Caroldong

2019-10-10T20:17:28Z

CHN-5：创建页面，内容为“== 英文原题 == GOTO [25 marks] The Gravitational-Wave Optical Transient Observer (GOTO) aims to carry out searches of optical counterparts of any Gravitational…”

2019-09-05T07:49:24Z

创建页面，内容为“== 英文原题 == GOTO [25 marks] The Gravitational-Wave Optical Transient Observer (GOTO) aims to carry out searches of optical counterparts of any Gravitational…”

新页面

== 英文原题 ==
GOTO [25 marks]

The Gravitational-Wave Optical Transient Observer (GOTO) aims to carry out searches of optical counterparts of any Gravitational Wave (GW) sources within an hour of their detection by the LIGO and VIRGO experiments. The survey needs to cover a big area on the sky in a short time to search all possible regions constrained by the GW experiments before the optical burst signal, if any, fades away. The GOTO telescope array is composed of 4 identical reflective telescopes, each with 40-cm diameter aperture and f-ratio of 2.5, working together to image large regions of the sky. For simplicity, we assume that the telescopes’ fields-of-view (FoV) do not overlap with one another.

a) Calculate the projected angular size per mm at the focal plane, i.e. plate scale, of each telescope. [6]

b) If the zero-point magnitude (i.e. the magnitude at which the count rate detected by the detector is 1 count per second) of the telescope system is 18.5 mag, calculate the minimum time needed to reach 21 mag at Signal-to-Noise Ratio (SNR) = 5 for a point source. We first assume that the noise is dominated by both the Read-Out Noise (RON) at 10 counts/pixel and the CCD dark (thermal) noise (DN) rate of 1 count/pix/minute. The CCDs used with the GOTO have a 6-micron pixel size and gain (conversion factor between photo-electron and data count) of 1. The typical seeing at the observatory site is around 1.0 arcsec. [8]

The Signal-to-Noise Ratio is defined as

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 The Signal-to-Noise Ratio is defined as
-$$ \text{SNR} \equiv $$
+\[ \text{SNR} \equiv \frac{\text{Total Source Count}}{\sqrt{\Sigma_{i}{ } \text{Noise}_{I}^{2}}}= \frac{\text{Total Source Count}}{\sqrt{\sigma_{\text{RON}}^{2}+\sigma_{\text{DN}}^{2}+\ldots}} \text{ , }\]

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 == 英文原题 ==
-（T10）GOTO [25 marks]
+'''(T10)GOTO [25 marks]'''
 The Gravitational-Wave Optical Transient Observer (GOTO) aims to carry out searches of optical counterparts of any Gravitational Wave (GW) sources within an hour of their detection by the LIGO and VIRGO experiments. The survey needs to cover a big area on the sky in a short time to search all possible regions constrained by the GW experiments before the optical burst signal, if any, fades away. The GOTO telescope array is composed of 4 identical reflective telescopes, each with 40-cm diameter aperture and f-ratio of 2.5, working together to image large regions of the sky. For simplicity, we assume that the telescopes’ fields-of-view (FoV) do not overlap with one another.