Hector: a high-multiplex survey instrument for spatially resolved galaxy spectroscopy

Lawrence, Jon; Bland-Hawthorn, Joss; Bryant, Julia J.; Brzeski, Jurek; Colless, Matthew; Croom, S. M.; Gers, Luke; Gilbert, James; Gillingham, Peter; Goodwin, Michael; Heijmans, Jeroen; Horton, Anthony; Ireland, Michael; Miziarski, Stan; Saunders, W.; Smith, Greg

doi:10.1117/12.925260

Cited by 19 publications

(15 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The M * − M h relation is shown to be complex (Guo et al 2010); future large IFS surveys (e.g. Hector, Lawrence et al 2012) are required to test whether the j * − j h relation takes a similar form.…”

Section: Discussionmentioning

confidence: 99%

Revisiting the Stellar Mass–Angular Momentum–Morphology Relation: Extension to Higher Bulge Fraction and the Effect of Bulge Type

Sweet

Fisher

Glazebrook

et al. 2018

ApJ

View full text Add to dashboard Cite

We present the relation between stellar specific angular momentum j * , stellar mass M * , and bulge-to-total light ratio β for THINGS, CALIFA and Romanowsky & Fall datasets, exploring the existence of a fundamental plane between these parameters as first suggested by Obreschkow & Glazebrook. Our best-fit M * − j * relation yields a slope of α = 1.03 ± 0.11 with a trivariate fit including β. When ignoring the effect of β, the exponent α = 0.56 ± 0.06 is consistent with α = 2/3 predicted for dark matter halos. There is a linear β − j * /M * relation for β 0.4, exhibiting a general trend of increasing β with decreasing j * /M * . Galaxies with β 0.4 have higher j * than predicted by the relation. Pseudobulge galaxies have preferentially lower β for a given j * /M * than galaxies that contain classical bulges. Pseudobulge galaxies follow a well-defined track in β − j * /M * space, consistent with Obreschkow & Glazebrook, while galaxies with classical bulges do not. These results are consistent with the hypothesis that while growth in either bulge type is linked to a decrease in j * /M * , the mechanisms that build pseudobulges seem to be less efficient at increasing bulge mass per decrease in specific angular momentum than those that build classical bulges.

show abstract

Section: Discussionmentioning

confidence: 99%

Revisiting the Stellar Mass–Angular Momentum–Morphology Relation: Extension to Higher Bulge Fraction and the Effect of Bulge Type

Sweet

Fisher

Glazebrook

et al. 2018

ApJ

View full text Add to dashboard Cite

show abstract

“…There have also been successful preliminary tests of using modified commercial AWGs for astronomical spectroscopy. 8,9 AWGs, along with other advances in the field of astrophotonics, such as photonic lanterns 10 to convert multimode fibers to single mode fibers, Bragg gratings (in-fiber 11 as well as on-chip 12 ) to suppress unwanted OH-emission background (in NIR) and high-efficiency fiber bundles for directly carrying the light from the telescope focal plane, 13 offer a complete high efficiency miniaturized solution for astronomical spectroscopy in NIR. This has a potential to be a paradigm shifting development for future ground-, balloon-and space-based telescopes.…”

Section: Arrayed Waveguide Gratings (Awgs)mentioning

confidence: 99%

Development of high-resolution arrayed waveguide grating spectrometers for astronomical applications: first results

Gatkine

Veilleux

et al. 2016

SPIE Proceedings

Self Cite

View full text Add to dashboard Cite

Astrophotonics is the next-generation approach that provides the means to miniaturize near-infrared (NIR) spectrometers for upcoming large telescopes and make them more robust and inexpensive. The target requirements for our spectrograph are: a resolving power of ∼3000, wide spectral range (J and H bands), free spectral range of about 30 nm, high on-chip throughput of about 80% (-1dB) and low crosstalk (high contrast ratio) between adjacent on-chip wavelength channels of less than 1% (-20 dB). A promising photonic technology to achieve these requirements is Arrayed Waveguide Gratings (AWGs). We have developed our first generation of AWG devices using a silica-on-silicon substrate with a very thin layer of Si 3 N 4 in the core of our waveguides. The waveguide bending losses are minimized by optimizing the geometry of the waveguides. Our first generation of AWG devices are designed for H band have a resolving power of ∼1500 and free spectral range of ∼ 10 nm around a central wavelength of 1600 nm. The devices have a footprint of only 12 mm × 6 mm. They are broadband (1450-1650 nm), have a peak on-chip throughput of about 80% (∼ -1 dB) and contrast ratio of about 1.5% (-18 dB). These results confirm the robustness of our design, fabrication and simulation methods. Currently, the devices are designed for Transverse Electric (TE) polarization and all the results are for TE mode. We are developing separate J-and H-band AWGs with higher resolving power, higher throughput and lower crosstalk over a wider free spectral range to make them better suited for astronomical applications.

show abstract

“…The work presented in this paper extends the investigation of Ho et al (2014Ho et al ( , 2016b and contributes to placing SAMI observations of wind-dominated galaxies in a physical context. Together, these studies provide important constraints for ongoing IFS surveys and, in the longer term, will help with planning for the next generation multi-object integral field units including HECTOR, the successor of SAMI (Lawrence et al 2012;Bland-Hawthorn 2015;Bryant et al 2016).…”

Section: Discussionmentioning

confidence: 99%

The SAMI Galaxy Survey: understanding observations of large-scale outflows at low redshift with EAGLE simulations

Tescari

Cortese

Power

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

This work presents a study of galactic outflows driven by stellar feedback. We extract main sequence disc galaxies with stellar mass 10 9 M /M 5.7 × 10 10 at redshift z = 0 from the highest resolution cosmological simulation of the Evolution and Assembly of GaLaxies and their Environments (EAGLE) set. Synthetic gas rotation velocity and velocity dispersion (σ) maps are created and compared to observations of disc galaxies obtained with the Sydney-AAO Multi-object Integral field spectrograph (SAMI), where σ-values greater than 150 km s −1 are most naturally explained by bipolar outflows powered by starburst activity. We find that the extension of the simulated edge-on (pixelated) velocity dispersion probability distribution depends on stellar mass and star formation rate surface density (Σ SFR ), with low-M /low-Σ SFR galaxies showing a narrow peak at low σ (∼ 30 km s −1 ) and more active, high-M /high-Σ SFR galaxies reaching σ > 150 km s −1 . Although supernova-driven galactic winds in the EAGLE simulations may not entrain enough gas with T < 10 5 K compared to observed galaxies, we find that gas temperature is a good proxy for the presence of outflows. There is a direct correlation between the thermal state of the gas and its state of motion as described by the σ-distribution. The following equivalence relations hold in EAGLE: i) low-σ peak ⇔ disc of the galaxy ⇔ gas with T < 10 5 K; ii) high-σ tail ⇔ galactic winds ⇔ gas with T 10 5 K.

show abstract

Hector: a high-multiplex survey instrument for spatially resolved galaxy spectroscopy

Cited by 19 publications

References 23 publications

Revisiting the Stellar Mass–Angular Momentum–Morphology Relation: Extension to Higher Bulge Fraction and the Effect of Bulge Type

Revisiting the Stellar Mass–Angular Momentum–Morphology Relation: Extension to Higher Bulge Fraction and the Effect of Bulge Type

Development of high-resolution arrayed waveguide grating spectrometers for astronomical applications: first results

The SAMI Galaxy Survey: understanding observations of large-scale outflows at low redshift with EAGLE simulations

Contact Info

Product

Resources

About