Prof Gavin Dalton: Publications

HiZELS: The High Redshift Emission Line Survey with UKIRT

Chapter in Thirty Years of Astronomical Discovery with UKIRT, Springer Nature 37 (2013) 235-250

Authors:

Philip Best, Ian Smail, David Sobral, Jim Geach, Tim Garn, Rob Ivison, Jaron Kurk, Gavin Dalton, Michele Cirasuolo, Mark Casali

The HiZELS/UKIRT Large Survey for Bright Lyα Emitters at z ∼ 9

Chapter in THIRTY YEARS OF ASTRONOMICAL DISCOVERY WITH UKIRT: THE SCIENTIFIC ACHIEVEMENT OF THE UNITED KINGDOM INFRARED TELESCOPE, 37 (2013) 251-258

Authors:

David Sobral, Philip Best, Jim Geach, Ian Smail, Jaron Kurk, Michele Cirasuolo, Mark Casali, Rob Ivison, Kristen Coppin, Gavin Dalton

The HiZELS/UKIRT Large Survey for Bright Lyα Emitters at z ∼ 9

Chapter in Thirty Years of Astronomical Discovery with UKIRT, Springer Nature 37 (2013) 251-258

Authors:

David Sobral, Philip Best, Jim Geach, Ian Smail, Jaron Kurk, Michele Cirasuolo, Mark Casali, Rob Ivison, Kristen Coppin, Gavin Dalton

Black hole mass and eddington ratio distribution functions of X-ray-selected broad-line AGNs at z ∼ 1.4 in the Subaru XMM-Newton Deep Field

Astrophysical Journal 761:2 (2012)

Authors:

K Nobuta, M Akiyama, Y Ueda, MG Watson, J Silverman, K Hiroi, K Ohta, F Iwamuro, K Yabe, N Tamura, Y Moritani, M Sumiyoshi, N Takato, M Kimura, T Maihara, G Dalton, I Lewis, D Bonfield, H Lee, E Curtis-Lake, E MacAulay, F Clarke, K Sekiguchi, C Simpson, S Croom, M Ouchi, H Hanami, T Yamada

Abstract:

In order to investigate the growth of supermassive black holes (SMBHs), we construct the black hole mass function (BHMF) and Eddington ratio distribution function (ERDF) of X-ray-selected broad-line active galactic nuclei (AGNs) at z ∼ 1.4 in the Subaru XMM-Newton Deep Survey (SXDS) field. A significant part of the accretion growth of SMBHs is thought to take place in this redshift range. Black hole masses of X-ray-selected broad-line AGNs are estimated using the width of the broad Mg II line and 3000 Å monochromatic luminosity. We supplement the Mg II FWHM values with the Hα FWHM obtained from our NIR spectroscopic survey. Using the black hole masses of broad-line AGNs at redshifts between 1.18 and 1.68, the binned broad-line AGN BHMFs and ERDFs are calculated using the V maxmethod. To properly account for selection effects that impact the binned estimates, we derive the corrected broad-line AGN BHMFs and ERDFs by applying the maximum likelihood method, assuming that the ERDF is constant regardless of the black hole mass. We do not correct for the non-negligible uncertainties in virial BH mass estimates. If we compare the corrected broad-line AGN BHMF with that in the local universe, then the corrected BHMF at z = 1.4 has a higher number density above 108 M⊙but a lower number density below that mass range. The evolution may be indicative of a downsizing trend of accretion activity among the SMBH population. The evolution of broad-line AGN ERDFs from z = 1.4 to 0 indicates that the fraction of broad-line AGNs with accretion rates close to the Eddington limit is higher at higher redshifts. © 2012. The American Astronomical Society. All rights reserved..

Development of the single fibres and IFUs of WEAVE

Proceedings of SPIE - The International Society for Optical Engineering 8450 (2012)

Authors:

I Guinouard, P Bonifacio, SC Trager, MAW Verheijen, I Lewis, G Dalton

Abstract:

WEAVE is a new wide-field spectroscopy facility proposed for the prime focus of the 4.2m William Herschel telescope. The facility comprises a new 2 degree field of view prime focus corrector with a 1000-multiplex fibre positioner, a small number of individually deployable IFUs, and a large single IFU. The IFUs and the MOS fibres can be used to feed a dual-beam spectrograph that will provide full coverage of the majority of the visible spectrum in a single exposure at a resolution ∼5000 or two 50nm-wide regions at a resolution of ∼20000. This paper sums up the design of these two modes and describes the specific developments required to optimise the performances of the fibre system. © 2012 SPIE.

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