High Time Resolution Astrophysics and Extremely Large Telescopes

Shearer, A.; Cunniffe, John; Voisin, Bruno; Neustroev, V.; Andersen, Torben; Enmark, Anita

doi:10.1063/1.2896933

Cited by 6 publications

(6 citation statements)

References 2 publications

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“…This also supports its correct optical identification. The X-ray and tentative optical parameters of J1124-5916 are very similar to the parameters of 3C 58 pulsar+PWN system, recently identified in the optical and mid-infrared (Shibanov et al, 2008;Slane et al, 2008;Shearer & Neustroev, 2008). The coincidence of the properties of these two PWNe is not surprising, since their pulsars have similar key parameters like the spindown luminosity and age.…”

Section: Discussionsupporting

confidence: 78%

A likely optical counterpart of the G292.0+1.8 pulsar wind nebula

Zharikov¹,

Shibanov

Zyuzin³

et al. 2008

A&A

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Context. G292.0+1.8 is the Cas A-like supernova remnant containing the young pulsar PSR J1124-5916, which powers a compact torus-like pulsar wind nebula with a jet visible in X-rays. Aims. We have performed deep optical observations of the pulsar field to detect the optical counterpart of the pulsar and its nebula. Methods. The observations were carried out using the direct imaging mode of FORS2 at the ESO VLT/UT1 telescope in the V, R, and I bands. We also analyzed archival images obtained with the Chandra/ACIS-I, ACIS-S, and HRC-S in X-rays. Results. In all three optical bands we detect a faint elliptical nebulosity, whose brightness peak and center position are consistent at a sub-arcsecond level with the X-ray position of the pulsar. The field is densely packed with background stars, but after subtraction of these stars the morphology of the object and the orientation of its major axis appear to be in a good agreement with the brightest inner part of the pulsar nebula torus region seen almost edge on in X-rays. Within the nebulosity we do not resolve any point-like optical object that could be identified with the pulsar and estimate its contribution to the observed nebulosity flux as < ∼ 20%. Extracting the X-ray spectrum from the physical region equivalent to the optical source position and extent and combining that with the measured optical fluxes, we compile a tentative multi-wavelength spectrum of the inner part of the nebula. Within uncertainties of the interstellar extinction towards G292.0+1.8 it is reminiscent of either the Crab or PSR B540-69 and J0205+6449 pulsar wind nebula spectra. Conclusions. The position, morphology, and spectral properties of the detected nebulosity suggest that it is the likely optical counterpart of the pulsar plus its wind nebula system in G292.0+1.8. Higher spatial resolution optical observations and the extension of the broad-band spectrum of the proposed counterpart candidate towards the IR and UV are necessary to confirm its origin.

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Section: Discussionsupporting

confidence: 78%

A likely optical counterpart of the G292.0+1.8 pulsar wind nebula

Zharikov¹,

Shibanov

Zyuzin³

et al. 2008

A&A

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“…Such phenomena include for example pulsars, close binary star systems, and stellar surface oscillations, etc. 17 The development of a ROIC capable or operating in a vacuum environment with a microchannel plate is a stepping stone to developing a wide range of detectors some of which have been identified immediately above.…”

Section: Enabling Technologymentioning

confidence: 99%

High event rate ROICs (HEROICs) for astronomical UV photon counting detectors

Harwit¹,

Argabright²,

Franka³

et al. 2014

SPIE Proceedings

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The next generation of astronomical photocathode / microchannel plate based UV photon counting detectors will overcome existing count rate limitations by replacing the anode arrays and external cabled electronics with anode arrays integrated into imaging Read Out Integrated Circuits (ROICs). We have fabricated a High Event Rate ROIC (HEROIC) consisting of a 32 by 32 array of 55 μm square pixels on a 60 μm pitch. The pixel sensitivity (threshold) has been designed to be globally programmable between 1 x 10 3 and 1 x 10 6 electrons. To achieve the sensitivity of 1 x 10 3 electrons, parasitic capacitances had to be minimized and this was achieved by fabricating the ROIC in a 65 nm CMOS process. The ROIC has been designed to support pixel counts up to 4096 events per integration period at rates up to 1 MHz per pixel. Integration time periods can be controlled via an external signal with a time resolution of less than 1 microsecond enabling temporally resolved imaging and spectroscopy of astronomical sources. An electrical injection port is provided to verify functionality and performance of each ROIC prior to vacuum integration with a photocathode and microchannel plate amplifier. Test results on the first ROICs using the electrical injection port demonstrate sensitivities between 3 x 10 3 and 4 x 10 5 electrons are achieved. A number of fixes are identified for a re-spin of this ROIC.

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“…The E-ELT will be able to identify ≈ 100 among the known radio pulsars through direct imaging and to measure their flux with unprecedented accuracy for objects this faint. In particular, the E-ELT, if equipped with high-time resolution instruments, will allow to detect Crab-like optical pulsars in M31 (Shearer 2010). The identification score will be large enough to perform population studies of the optically-identified INSs and to investigate, on a much larger statistics, the dependence of their optical emission properties on the pulsar parameters (e.g., age, period, magnetic field).…”

Section: The Role Of the E-elt In Neutron Star Astronomymentioning

confidence: 99%

Neutron Star Astronomy with the E-ELT

Mignani¹

2010

Preprint

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So far, 24 Isolated neutron stars (INSs) of different types have been identified at optical wavelengths, from the classical radio pulsars to more peculiar objects, like the magnetars. Most identifications have been obtained in the last 20 years thanks to the deployment of modern technology telescopes, above all the HST, but also the NTT and, later, the 8m-class telescopes like the VLT. The larger identification rate has increased the impact factor of optical observations in the multi-wavelength approach to INS astronomy, opening interesting possibilities for studies not yet possible at other wavelengths. With the HST on the way to its retirement, 8m class telescopes will have the task of bridging neutron star optical astronomy into a new era, characterised by the advent of the generation of extremely large telescopes (ELTs), like the European ELT (E-ELT). This will mark a major step forward in the field, enabling one to identify many more INSs, many of which from follow-ups of observations performed with future radio and X-ray megastruscture facilities like SKA and IXO. Moreover, the E-ELT will make it possible to carry out observations, like timing, spectroscopy, and polarimetry, which still represent a challenge for 8m-class telescopes and are, in many respects, crucial for studies on the structure and composition of the neutron star interior and of its magnetosphere. In this contribution, I briefly summarise the current status of INS optical observations, describe the main science goals for the E-ELT, and their impact on neutron star physics.

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High Time Resolution Astrophysics and Extremely Large Telescopes

Cited by 6 publications

References 2 publications

A likely optical counterpart of the G292.0+1.8 pulsar wind nebula

A likely optical counterpart of the G292.0+1.8 pulsar wind nebula

High event rate ROICs (HEROICs) for astronomical UV photon counting detectors

Neutron Star Astronomy with the E-ELT

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