Hexabundles: imaging fiber arrays for low-light astronomical applications

Bland-Hawthorn, Joss; Bryant, Julia J.; Robertson, Gordon; Gillingham, Peter; O’Byrne, John W.; Cecil, Gerald; Haynes, Roger; Croom, S. M.; Ellis, S. C.; Maack, Martin D.; Skovgaard, Peter M. W.; Noordegraaf, Danny

doi:10.1364/oe.19.002649

Cited by 162 publications

(110 citation statements)

References 15 publications

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“…SAMI provides a multiplex of ×13 with each integralfield unit (IFU) having a diameter of 15 arcsec and uses compact fused fibre bundles with minimised cladding between the fibre cores (hexabundles: Bland-Hawthorn et al 2011;Bryant et al 2011Bryant et al , 2014. The MaNGA Survey operating on the Apache Point 2.3m Telescope, has also begun a similar project, with an IFU multiplex of ×16.…”

Section: Hill 2014mentioning

confidence: 99%

“…The SAMI instrument SAMI is mounted at the prime focus of the AngloAustralian Telescope and has 1-degree-diameter field of view. SAMI uses 13 fused optical fibre bundles (hexabundles; Bland-Hawthorn et al 2011;Bryant et al 2011Bryant et al , 2014) with a high (75 percent) fill factor. Each bundle combines 61 optical fibres of 1.6 arcsec diameter to form an IFU of 15-arcsec diameter.…”

Section: Hill 2014mentioning

confidence: 99%

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The SAMI Galaxy Survey: Data Release One with emission-line physics value-added products

Green

Croom

Scott

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the first major release of data from the SAMI Galaxy Survey. This data release focuses on the emission-line physics of galaxies. Data Release One includes data for 772 galaxies, about 20% of the full survey. Galaxies included have the redshift range 0.004 < z < 0.092, a large mass range (7.6 < log M * / M < 11.6), and star-formation rates of ∼ 10 −4 to ∼ 10 1 M yr −1 . For each galaxy, we include two spectral cubes and a set of spatially resolved 2D maps: single-and multicomponent emission-line fits (with dust extinction corrections for strong lines), local dust extinction and star-formation rate. Calibration of the fibre throughputs, fluxes and differential-atmosphericrefraction has been improved over the Early Data Release. The data have average spatial resolution of 2.16 arcsec (FWHM) over the 15 arcsec diameter field of view and spectral (kinematic) resolution R = 4263 (σ = 30 km s −1 ) around Hα. The relative flux calibration is better than 5% and absolute flux calibration better than ±0.22 mag, with the latter estimate limited by galaxy photometry. The data are presented online through the Australian Astronomical Observatory's Data Central.

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Section: Hill 2014mentioning

confidence: 99%

Section: Hill 2014mentioning

confidence: 99%

The SAMI Galaxy Survey: Data Release One with emission-line physics value-added products

Green

Croom

Scott

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…For example, the Calar Alto Legacy Integral Field Area survey will obtain spatially resolved spectroscopic information for about 600 galaxies in the local universe, using integral field spectroscopy (Sánchez et al 2012). New imaging fiber bundles (so called hexabundles) are to be used on widefield survey telescopes (e.g., AAT; Bland-Hawthorn et al 2011;Croom et al 2012) to obtain spatially resolved stellar and gas kinematics for a volume-limited sample 10 4-5 galaxies. With such surveys it will be possible to study the AMD of galaxies in voids, filaments, groups, and clusters.…”

Section: Introductionmentioning

confidence: 99%

On the Origin of the Angular Momentum Properties of Gas and Dark Matter in Galactic Halos and Its Implications

Sharma

Steinmetz

Bland-Hawthorn

2012

ApJ

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We perform a set of non-radiative hydrodynamical simulations of merging spherical halos in order to understand the angular momentum (AM) properties of the galactic halos seen in cosmological simulations. The universal shape of AM distributions seen in simulations is found to be generically produced as a result of mergers. The universal shape is such that it has an excess of low AM material and hence cannot explain the exponential structure of disk galaxies. A resolution to this is suggested by the spatial distribution of low AM material which is found to be in the center and a conical region close to the axis of rotation. A mechanism that preferentially discards the material in the center and prevents the material along the poles from falling onto the disk is proposed as a solution. We implement a simple geometric criterion for the selective removal of low AM material and show that in order for 90% of halos to host exponential disks one has to reject at least 40% of material. Next, we explore the physical mechanisms responsible for distributing the AM within the halo during a merger. For dark matter there is an inside-out transfer of AM, whereas for gas there is an outside-in transfer, which is due to differences between collisionless and gas dynamics. This is responsible for the spin parameter λ and the shape parameter α of AM distributions being higher for gas compared to dark matter. We also explain the apparent high spin of dark matter halos undergoing mergers and show that a criterion stricter than what is currently used would be required to detect such unrelaxed halos. Finally, we demonstrate that the misalignment of AM between gas and dark matter only occurs when the intrinsic spins of the merging halos are not aligned with the orbital AM of the system. The self-misalignment (orientation of AM when measured in radial shells not being constant), which could be the cause of warps and anomalous rotation in disks galaxies, also occurs under similar conditions. The frequency and amplitude of this misalignment are roughly consistent with the properties of warps seen in disk galaxies.

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“…Improvements in manufacturing and assembly techniques have steadily reduced each of these problems. The use of multimode fibers increased coupling efficiency, 72 as did the use of lenslets registered to each fiber so that the light is focused onto the fiber cores and not in regions with poor coupling efficiency. (Lee et al mention that these fiber-coupling lenslets should be used at f∕4 to f∕6.…”

Section: Integral Field Spectrometry With Coherent Fiber Bundles (Ifsmentioning

confidence: 99%

Review of snapshot spectral imaging technologies

2013

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Within the field of spectral imaging, the vast majority of instruments used are scanning devices. Recently, several snapshot spectral imaging systems have become commercially available, providing new functionality for users and opening up the field to a wide array of new applications. A comprehensive survey of the available snapshot technologies is provided, and an attempt has been made to show how the new capabilities of snapshot approaches can be fully utilized. © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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Hexabundles: imaging fiber arrays for low-light astronomical applications

Cited by 162 publications

References 15 publications

The SAMI Galaxy Survey: Data Release One with emission-line physics value-added products

The SAMI Galaxy Survey: Data Release One with emission-line physics value-added products

On the Origin of the Angular Momentum Properties of Gas and Dark Matter in Galactic Halos and Its Implications

Review of snapshot spectral imaging technologies

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