The Sydney-AAO Multi-object Integral field spectrograph

Croom, S. M.; Lawrence, Jon; Bland-Hawthorn, Joss; Bryant, Julia J.; Fogarty, L. M. R.; Richards, Samuel N.; Goodwin, Michael; Farrell, Tony; Miziarski, Stan; Heald, Ron; Jones, D. Heath; Lee, Stephen; Colless, Matthew; Brough, Sarah; Hopkins, A. M.; Bauer, A.; Birchall, Michael; Ellis, S. C.; Horton, Anthony; Leon-Saval, Sergio G.; Lewis, Geraint F.; López-Sánchez, Á. R.; Min, Sung-Hwan; Trinh, Christopher; Trowland, Holly

doi:10.1111/j.1365-2966.2011.20365.x

Cited by 425 publications

(312 citation statements)

References 158 publications

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“…These components are consistent with a photometric bulge-disk decomposition. Ideally such procedure could be carried out on large numbers of galaxies in forthcoming data releases of SAMI (Croom et al, 2012) and MaNGA (Bundy et al, 2014). However, its not clear that either survey has sufficient spatial or spectral resolution to apply this technique.…”

Section: Definition Of a Bulgementioning

confidence: 99%

An Observational Guide to Identifying Pseudobulges and Classical Bulges in Disc Galaxies

Fisher¹,

Drory²

2016

Astrophysics and Space Science Library

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In this review our aim is to summarize the observed properties of pseudobulges and classical bulges. We utilize an empirical approach to studying the properties of bulges in disk galaxies, and restrict our analysis to statistical properties. A clear bimodality is observed in a number of properties including morphology, structural properties, star formation, gas content & stellar population, and kinematics. We conclude by summarizing those properties that isolate pseudobulges from classical bulges. Our intention is to describe a practical, easy to use, list of criteria for identifying bulge types.

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Section: Definition Of a Bulgementioning

confidence: 99%

An Observational Guide to Identifying Pseudobulges and Classical Bulges in Disc Galaxies

Fisher¹,

Drory²

2016

Astrophysics and Space Science Library

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“…Recent advances now enable multiobject IFS with instruments such as SAMI (Croom et al 2012), KMOS (Sharples et al 2013), and MaNGA (Mapping Nearby Galaxies at Apache Point Observatory; Drory et al 2015). As a part of the 4th generation of the Sloan Digital Sky Survey (SDSS-IV), the MaNGA project bundles fibers from the Baryon Oscillation Spectroscopic Survey (BOSS) spectrograph (Smee et al 2013) into integral-field units (IFUs) to obtain spatially resolved optical spectroscopy of 10,000 nearby galaxies over a 6 year survey.…”

Section: Introductionmentioning

confidence: 99%

“…The reconstructed image of such unresolved objects can either look small and circular (if the object was centered on a single fiber), large and circular (if the object was centered in the interstitial gap between three fibers), highly elongated (if the object was centered midway between two fibers), along with any range of shapes in between. This is highly undesirable from a science standpoint, and therefore typical fiber-bundle IFU surveys (e.g., Croom et al 2012;Sánchez et al 2012) dither their observations. Small dithers of a fraction of the fiber spacing sample the missing points in the image plane and allow reconstructed images based on multiple, dithered exposures to achieve fairly uniform and integral spatial coverage.…”

Section: Introductionmentioning

confidence: 99%

OBSERVING STRATEGY FOR THE SDSS-IV/MaNGA IFU GALAXY SURVEY

Law¹,

Yan²,

Bershady³

et al. 2015

385

333

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Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) is an integral-field spectroscopic survey that is one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV). MaNGA's 17 pluggable optical fiber-bundle integral field units (IFUs) will observe a sample of 10,000 nearby galaxies distributed throughout the SDSS imaging footprint (focusing particularly on the North Galactic Cap). In each pointing these IFUs are deployed across a 3°field; they yield spectral coverage 3600−10300 Å at a typical resolution R ∼ 2000, and sample the sky with 2″ diameter fiber apertures with a total bundle fill factor of 56%. Observing over such a large field and range of wavelengths is particularly challenging for obtaining uniform and integral spatial coverage and resolution at all wavelengths and across each entire fiber array. Data quality is affected by the IFU construction technique, chromatic and field differential refraction, the adopted dithering strategy, and many other effects. We use numerical simulations to constrain the hardware design and observing strategy for the survey with the aim of ensuring consistent data quality that meets the survey science requirements while permitting maximum observational flexibility. We find that MaNGA science goals are best achieved with IFUs composed of a regular hexagonal grid of optical fibers with rms displacement of 5 μm or less from their nominal packing position; this goal is met by the MaNGA hardware, which achieves 3 μm rms fiber placement. We further show that MaNGA observations are best obtained in sets of three 15 minute exposures dithered along the vertices of a 1.44 arcsec equilateral triangle; these sets form the minimum observational unit, and are repeated as needed to achieve a combined signal-to-noise ratio of 5 Å −1 per fiber in the r-band continuum at a surface brightness of 23 AB arcsec −2 . In order to ensure uniform coverage and delivered image quality, we require that the exposures in a given set be obtained within a 60 minute interval of each other in hour angle, and that all exposures be obtained at airmass 1.2  (i.e., within 1-3 hr of transit depending on the declination of a given field).

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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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The Sydney-AAO Multi-object Integral field spectrograph

Cited by 425 publications

References 158 publications

An Observational Guide to Identifying Pseudobulges and Classical Bulges in Disc Galaxies

An Observational Guide to Identifying Pseudobulges and Classical Bulges in Disc Galaxies

OBSERVING STRATEGY FOR THE SDSS-IV/MaNGA IFU GALAXY SURVEY

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

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