The Liverpool Telescope: performance and first results

Steele, I. A.; Smith, R. J.; Rees, Philippa; Baker, Ian P.; Bates, Stuart; Bode, M. F.; Bowman, Mark; Carter, Dave; Etherton, J.; Ford, M.; Fraser, S. N.; Gomboc, A.; Lett, Robert D. J.; Mansfield, Anthony G.; Marchant, J. M.; Medrano-Cerda, Gustavo A.; Mottram, Christopher J.; Raback, D.; Scott, A. B.; Tomlinson, M. D.; Zamanov, R.

doi:10.1117/12.551456

Cited by 294 publications

(95 citation statements)

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“…A few tens of transient candidates identified by the widefield telescopes were followed up on the 10 m Keck II telescope (using the DEIMOS instrument; Faber et al 2003), the 2 m Liverpool Telescope (LT; Steele et al 2004), the Palomar 200 inch Hale telescope (P200; Bracher 1998), the 3.6 m ESO New Technology Telescope (within the Public ESO Spectroscopic Survey of Transient Objects, PESSTO; Smartt et al 2015), and the University of Hawaii 2.2 m telescope (SuperNovae Integral Field Spectrograph, SNIFS). The follow-up observations of the candidate counterparts are summarized in Table 3 of the main paper.…”

Section: Optical and Near-ir Observationsmentioning

confidence: 99%

SUPPLEMENT: “LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW150914” (2016, ApJL, 826, L13)

Abbott¹,

Abbott²,

Abbott³

et al. 2016

ApJS

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This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.

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Section: Optical and Near-ir Observationsmentioning

confidence: 99%

SUPPLEMENT: “LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW150914” (2016, ApJL, 826, L13)

Abbott¹,

Abbott²,

Abbott³

et al. 2016

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“…RINGO3 (Arnold et al 2012) is a fast-readout optical imaging polarimeter at the Liverpool Telescope (Steele et al 2004). Unlike the original RINGO 2 which used deviating optics to spread the time varying polarised signal into rings, RINGO3 uses a fast readout camera to capture this signal as it changes in time.…”

Section: Ringo3 Polarimetermentioning

confidence: 99%

Calibration of the Liverpool Telescope RINGO3 polarimeter

Słowikowska

Krzeszowski

Żejmo

et al. 2016

Mon. Not. R. Astron. Soc.

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We present an analysis of polarimetric observations of standard stars performed over the period of more than three years with the RINGO3 polarimeter mounted on the Liverpool Telescope. The main objective was to determine the instrumental polarisation of the RINGO3 polarimeter in three spectral energy ranges: blue (350-640 nm), green (650-760 nm) and red (770-1000 nm). The observations were conducted between 2012 and 2016. The total time span of 1126 days was split into five epochs due to the hardware changes to the observing system. Our results should be applied to calibrate all polarimetric observations performed with the RINGO3 polarimeter.

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“…We observed Swift J1357.2-0933 with the IO:O camera attached to the 2m Liverpool Telescope in La Palma, Spain (Steele et al 2004). Our observations were carried out ∼ 30 months after the outburst on 2013 Jul 9 (4 × 300s), Jul 10 (4 × 300s; these were simultaneous with our XMM-Newton observation) and Jul 12 (3 × 300s), using the Sloan r ′ filter.…”

Section: Optical Observationsmentioning

confidence: 99%

Swift J1357.2−0933: the faintest black hole?

Padilla¹,

Wijnands

Degenaar³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Swift J1357.2-0933 is a confirmed very faint black hole X-ray transient and has a short estimated orbital period of 2.8 hr. We observed Swift J1357.2-0933 for ∼50 ks with XMM-Newton in 2013 July during its quiescent state. The source is clearly detected at a 0.5-10 keV unabsorbed flux of ∼ 3 × 10 −15 erg cm −2 s −1 . If the source is located at a distance of 1.5 kpc (as suggested in the literature), this would imply a luminosity of ∼ 8 × 10 29 erg s −1 , making it the faintest detected quiescent black hole LMXB. This would also imply that there is no indication of a reversal in the quiescence Xray luminosity versus orbital period diagram down to 2.8 hr, as has been predicted theoretically and recently supported by the detection of the 2.4 hr orbital period black hole MAXI J1659-152 at a 0.5-10 keV X-ray luminosity of ∼ 1.2 × 10 31 erg s −1 . However, there is considerable uncertainty in the distance of Swift J1357.2-0933 and it may be as distant as 6.3 kpc. In this case, its quiescent luminosity would be L X ∼ 1.3 × 10 31 erg s −1 , i.e., similar to MAXI J1659-152 and hence it would support the existence of such a bifurcation period. We also detected the source in optical at r ′ ∼22.3 mag with the Liverpool telescope, simultaneously to our X-ray observation. The Xray/optical luminosity ratio of Swift J1357.2-0933 agrees with the expected value for a black hole at this range of quiescent X-ray luminosities.

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The Liverpool Telescope: performance and first results

Cited by 294 publications

References 0 publications

SUPPLEMENT: “LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW150914” (2016, ApJL, 826, L13)

SUPPLEMENT: “LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW150914” (2016, ApJL, 826, L13)

Calibration of the Liverpool Telescope RINGO3 polarimeter

Swift J1357.2−0933: the faintest black hole?

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