UFTI: the 0.8 - 2.5 μm fast track imager for the UK infrared telescope

Roche, P. F.; Lucas, P. W.; Mackay, Craig D.; Ettedgui-Atad, Eli; Hastings, Peter; Bridger, Alan; Rees, Nicholas P.; Leggett, S. K.; Davis, Chris; Holmes, A.; Handford, T.

doi:10.1117/12.460987

Cited by 33 publications

(6 citation statements)

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“…We obtained classical narrow-band imaging of two SMGs, SMM J105226.61 and SMM J131232.31, whose redshifts should place Hα emission in the Brγ and H 2 S1 filters, respectively. These data were taken with the UFTI near-infrared camera (Roche et al 2003) on UKIRT 6 on 2003 February 25-27 in < ∼ 0.7 ′′ seeing and photometric conditions. The UFTI camera has a 1024 × 1024 HgCdTe array and a plate scale of 0.091 ′′ pixel −1 , giving a field of view of 92 ′′ ×92 ′′ (which probes roughly 0.75 Mpc in our adopted cosmology).…”

Section: Uftimentioning

confidence: 99%

The Rest‐Frame Optical Spectra of SCUBA Galaxies

Swinbank

Smail

Chapman

et al. 2004

ApJ

291

511

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We present near-infrared spectroscopy and narrow-band imaging at the wavelength of redshifted Hα for a sample of 30 high-redshift, far-infrared luminous galaxies. This sample is selected from surveys in the submillimeter, millimeter and radio wavebands and has complete redshift coverage with a median redshift of z ∼ 2.4. We use our data to measure the Hα properties of these systems and to gauge the prevalence of active galactic nuclei (AGN) in these galaxies through their [NII]/Hα ratios and Hα line widths. Removing obvious AGN, we find that the predicted Hα star formation rates in this diverse population are suppressed (by a factor of ∼ 10) compared to those derived from their far-infrared luminosities. Using the AGN indicators provided by our nearinfrared spectra, we estimate that AGN are present in at least 40% of the galaxies in our sample. To further investigate this, we construct a composite rest-frame spectrum for both the entire sample and for those galaxies which individually show no signs of nuclear activity. We find [NII]/Hα ratios for both composite spectra which suggest that the energy output of the galaxies is star-formation-rather than AGN-dominated. However, we also find that the Hα line in the composite non-AGN spectrum is best fit with an underlying broad-line component with a narrow/broad flux ratio of 0.45 ± 0.20. The median Hα line width for our sample (removing obvious AGN) is 400 ± 70 km s −1 (FWHM), and the typical spatial extent of the Hα emission in our narrow-band observations is < ∼ 4-8 kpc, which indicates a dynamical mass of 1-2×10 11 M ⊙ with corresponding dynamical times of 10-20 Myr. Using both high-resolution imaging and spectroscopically identified velocity offsets, we find that seven of the far-infrared luminous galaxies have companions, suggesting that they are undergoing interactions/mergers and from their relative velocities we can determine a dynamical mass of 1.5 ± 0.9 × 10 11 M ⊙ . These measurements are comparable to millimeter CO estimates for the dynamical masses of these systems on similar scales, and larger than recent estimates of the dynamical masses of UV-selected galaxies at similar redshifts derived in an identical manner. Using the [NII]/Hα index to predict abundances, we investigate the Luminosity-Metallicity relation for these galaxies and find that many have metallicities consistent with UV-selected high-redshift galaxies and slightly lower than local luminous infrared and elliptical galaxies (although we caution that our metallicity estimates have possible systematic uncertainties). We also compared our Hα and far-infrared luminosities with deep Chandra observations of a subset of our survey fields and use these data to further assess their AGN content. We conclude that these high-redshift, far-infrared luminous galaxies represent a population of massive, metal-rich, merging systems with high instantaneous star formation rates, strong dust obscuration and actively-fueled AGN which are likely to be the progenitors of massive local elliptical galaxies.

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Section: Uftimentioning

confidence: 99%

The Rest‐Frame Optical Spectra of SCUBA Galaxies

Swinbank

Smail

Chapman

et al. 2004

ApJ

291

511

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“…In every case the follow‐up image was used as the reference image for the coordinate transform. Follow‐up images were obtained from a variety of instruments, including the UKIRT Fast‐Track Imager (UFTI; see Roche et al 2003), the Long‐slit Intermediate Resolution Infrared Spectrograph (LIRIS; see Manchado et al 2003), the WFCAM on UKIRT (see Casali et al 2007), the ESO Multi‐Mode Instrument (EMMI; see Dekker, Delabre & Dodorico 1986) and the ESO Faint Object Spectrograph and Camera (EFOSC2; see Buzzoni et al 1984).…”

Section: Proper Motionsmentioning

confidence: 99%

Blue not brown: UKIRT Infrared Deep Sky Survey T dwarfs with suppressed K-band flux

Murray

Burningham

Jones

et al. 2011

Monthly Notices of the Royal Astronomical Society

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The definitive version can be found at: http://onlinelibrary.wiley.com/ Copyright Royal Astronomical SocietyWe have used blue near-infrared colours to select a group of 12 spectroscopically confirmed United Kingdom InfraRed Telescope (UKIRT) Infrared Deep Sky Survey (UKIDSS) T dwarfs later than T4. From amongst these, we identify the first two kinematic halo T-dwarf candidates. Blue near-infrared colours have been attributed to collisionally induced hydrogen absorption, which is enhanced by either high surface gravity or low metallicity. Proper motions are measured and distances estimated, allowing the determination of tangential velocities. U and V components are estimated for our objects by assuming V-rad = 0. From this, ULAS J0926+0835 is found to have U = 62 km s(-1) and V = -140 km s(-1), and ULAS J1319+1209 is found to have U = 192 km s(-1) and V = -92 km s(-1). These values are consistent with potential halo membership. However, these are not the bluest objects in our selection. The bluest is ULAS J1233+1219, with J - K = -1.16 +/- 0.07, and surprisingly this object is found to have young disc-like U and V. Our sample also contains Hip 73786B, companion to the metal-poor K5 dwarf Hip 73786. Hip 73786 is a metal-poor star, with [Fe/H] = -0.3 +/- 0.1 and is located at a distance of 19 +/- 0.7 pc. U, V, W space velocity components are calculated for Hip 73786A and B, finding that U = -48 +/- 7 km s(-1), V = -75 +/- 4 km s(-1) and W = -44 +/- 8 km s(-1). From the properties of the primary, Hip 73786B is found to be at least 1.6-Gyr old. As a metal-poor object, Hip 73786B represents an important addition to the sample of known T dwarf benchmarks

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“…The data reduction part of the project was labelled ORAC-DR 14,15 and the aim was to provide an infrastructure for data processing using reusable processing blocks, called primitives, that represent high-level concepts such as "flatfield these images" or "combine into a single image", and are combined into "recipes". The system is designed to be completely generic and to ensure this the initial development included support for CGS4 and UFTI 16 at UKIRT and SCUBA at JCMT. The overall design is shown in Fig.…”

Section: Data Pipelinesmentioning

confidence: 99%

Data Management At the UKIRT and JCMT

Jenness¹,

Economou²

2011

Preprint

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For more than a decade the Joint Astronomy Centre has been developing software tools to simplify observing and make it possible to use the telescopes in many different operational modes. In order to support remote operations the data handling systems need to be in place to allow observation preparation, flexible queue scheduling, data quality pipelines and science archives all to be connected in a data-driven environment. We discuss the history of these developments at UKIRT and JCMT and how the decision to combine software development at both telescopes led each to get features that they could not have justified if they were treated independently.

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UFTI: the 0.8 - 2.5 μm fast track imager for the UK infrared telescope

Cited by 33 publications

References 0 publications

The Rest‐Frame Optical Spectra of SCUBA Galaxies

The Rest‐Frame Optical Spectra of SCUBA Galaxies

Blue not brown: UKIRT Infrared Deep Sky Survey T dwarfs with suppressed K-band flux

Data Management At the UKIRT and JCMT

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