In-orbit performance of the COSTAR-corrected Faint Object Camera

Jędrzejewski, R.; Hartig, G.; Jakobsen, P.; Crocker, J.; Ford, H. C.

doi:10.1086/187581

Cited by 10 publications

(5 citation statements)

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“…We obtained post-COSTAR Faint Object Camera (FOC) f/96 (Jedrzejewski et al 1994) images of 3C 279 from the HST archive with 'on-the-fly' pipeline calibration applied. Single high quality exposures with the F253M and F550M filters (each ∼1 ksec) were taken consecutively during November 1995 as part of a program (ID 6057) to study the inner structure of the quasar (Hook, Schreier, & Miley 2000) with the Fine Guidance Sensors (FGS) -see Table 1.…”

Section: Description Of Archival Observationsmentioning

confidence: 99%

Detection of Optical Synchrotron Emission from the Radio Jet of 3C 279

Cheung

2002

The Astrophysical Journal

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We report the detection of optical and ultraviolet emission from the kiloparsec-scale jet of the well-known quasar 3C 279. A bright knot, discovered in archival V-and U-band Hubble Space Telescope Faint Object Camera images, is coincident with a peak in the radio jet ∼0Љ .6 from the nucleus. The detection was also confirmed in Wide Field Planetary Camera 2 images. Archival Very Large Array and MERLIN radio data are also analyzed, and these data help to show that the high-energy optical/UV continuum and the spectrum are consistent with a synchrotron origin from the same population of relativistic electrons responsible for the radio emission.

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Section: Description Of Archival Observationsmentioning

confidence: 99%

Detection of Optical Synchrotron Emission from the Radio Jet of 3C 279

Cheung

2002

The Astrophysical Journal

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“…M15 was observed by HST on 27 September 1994, with the COSTAR optical correction system in place. (For details of the design and performance of the camera and correction system, see Greenfield et al 1991 andJedrzejewski et al 1994. ) Three ∼ 7 × 7-arcsecond FOC images were taken through each of the F430W (FOC "B") and F480LP (FOC "V ") filters; the exposure times ranged from 2020.75 to 2519.75 seconds.…”

Section: Observationsmentioning

confidence: 99%

Deep HST/FOC Imaging of the Central Density Cusp of the Globular Cluster M15

Sosin¹,

King²

1997

The Astronomical Journal

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Using the Faint Object Camera on the repaired Hubble Space Telescope, we have observed two fields in the globular cluster M15: the central density cusp, and a field at r = 20 ′′ . These are the highest-resolution images ever taken of this cluster's dense core, and are the first to probe the distribution of stars well below the main-sequence turnoff. After correction for incompleteness, we measure a logarithmic cusp slope (d log σ/d log r) of −0.70 ± 0.05 (1-sigma) for turnoff (∼ 0.8M ⊙ ) stars over the radial range from 0. ′′ 3 to 10 ′′ ; this slope is consistent with previous measurements. We also set an approximate upper limit of ∼ 1. ′′ 5 (90% confidence limit) on the size of any possible constant-surface-density core, but discuss uncertainties in this limit that arise from crowding corrections. We find that fainter stars in the cusp also have power-law density profiles: a mass group near 0.7M ⊙ has a logarithmic slope of −0.56 ± 0.05 (1-sigma) over the radial range from 2 ′′ to 10 ′′ . Taken together, the two slopes are not well matched by the simplest core-collapse or black-hole models. We also measure a mass function at r = 20 ′′ , outside of the central cusp. Both of the FOC fields show substantial mass segregation, when compared with a mass function measured with the WFPC2 at r = 5 ′ . In comparing the overall mass functions of the two FOC fields and the r = 5 ′ field, we find that the radial variation of the mass function is somewhat less than that predicted by a King-Michie model of the cluster, but greater than that predicted by a Fokker-Planck model taken from the literature.

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“…The PSF has two origins. One is spherical aberration and so on from the mirror figure, which as an isolated effect, could in principle be corrected using customized secondary mirrors, as was done in the Hubble Space Telescope (see figs 1-3 in Jedrzejewski et al 1994). However, the other contribution to the PSF is the roughness of the mirror surfaces, which cannot be compensated for and is a limiting factor that also prohibits the 1 For a month, we assume 30 × 12 h of observing time.…”

Section: Observation Time Calculationsmentioning

confidence: 99%

Towards a polarization prediction for LISA via intensity interferometry

Baumgartner

Bernardini

Cuissa

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Compact Galactic binary systems with orbital periods of a few hours are expected to be detected in gravitational waves (GW) by LISA or a similar mission. At present, these so-called verification binaries provide predictions for GW frequency and amplitude. A full polarisation prediction would provide a new method to calibrate LISA and other GW observatories, but requires resolving the orientation of the binary on the sky, which is not currently possible. We suggest a method to determine the elusive binary orientation and hence predict the GW polarisation, using km-scale optical intensity interferometry. The most promising candidate is CD–30○ 11223, consisting of a hot helium subdwarf with mB = 12 and a much fainter white dwarf companion, in a nearly edge-on orbit with period 70.5 min. We estimate that the brighter star is tidally stretched by 6%. Resolving the tidal stretching would provide the binary orientation. The resolution needed is far beyond any current instrument, but not beyond current technology. We consider scenarios where an array of telescopes with km-scale baselines and/or the Very Large Telescope (VLT) and Extremely Large Telescope (ELT) are equipped with recently-developed kilo-pixel sub-ns single-photon counters and used for intensity interferometry. We estimate that a team-up of the VLT and ELT could measure the orientation to ±1○ at 2σ confidence in 24 hours of observation.

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In-orbit performance of the COSTAR-corrected Faint Object Camera

Cited by 10 publications

References 0 publications

Detection of Optical Synchrotron Emission from the Radio Jet of 3C 279

Detection of Optical Synchrotron Emission from the Radio Jet of 3C 279

Deep HST/FOC Imaging of the Central Density Cusp of the Globular Cluster M15

Towards a polarization prediction for LISA via intensity interferometry

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