1. Julia Bryant HECTOR project scientist Australian Astronomical Observatory University of Sydney CAASTRO With Joss Bland-Hawthorn, Jon Lawrence, Scott Croom and the Hector team HECTOR - a massive new IFS instrument for the Anglo- Australian Telescope

2. SAMI Galaxy Survey Colours: N[II]/Hα Local density | environment | inclination | stochastic variation and precision Public data release of ~800 galaxies in July: http://sami-survey.org/

3. Decipher the diversity of galaxies through understanding the physical basis for their individuality. Physical drivers Mass and local environmentAccretion and merger history  morphology and star formation history. Large-scale environment  modulate galaxy growth through tidal torques and gas accretion. Measurables: Spin parameters, specific stellar angular momentum => merger histories Higher-order kinematics of the line-of-sight velocity distribution => formation paths Measure current kinematic disturbance as a probe of ongoing dynamical interactions Gas/stellar misalignment, metallicity gradients => external gas accretion Voids Groups Clusters Filaments Sheets

4. HECTOR Bryant et al. 2016 Bland-Hawthorn et al. 2015 Lawrence et al. 2012 Aim: Volume-limited IFS survey of >50,000 galaxies The next major dark time instrument for AAT. Staged build – Hector-I science operations by late-2018. Based on new or expanded technology concepts. 1.New improved hexabundle fibre IFUs 2.New positioning technology 3.New fixed-format replicable spectrographs

5. Hexabundles – optical fibre IFUs Hexabundles 61 optical fibres fused together using our glass fibre processing unit in the SAIL astrophotonics labs at Sydney University. Advantages of this design: Fill fraction ~75%. Low cross-talk < 0.5% Low focal ratio degradation (Bryant et al. 2011,2012,2014,2015) 1mm

6. What can be improved? Fibre configuration Larger sizes to cover 2 x R e in 90% of galaxies: 61-217 cores 15-30” New developments in hexabundles

7. Positioning New positioning technology to configure ~50 hexabundles across the field plate.

8. HECTOR spectrographs Benefits of high resolution Velocity dispersion Relative number 2.75 Å 1.3 Å 1.1 Å Stellar Continuum Science: SAMI: blue: R λ = 2.7Å (R~1800) red: R λ = 1.6Å (R~4300) MANGA: blue: R λ = 2.85Å red: R λ = 3.4Å R λ [Å] ≤ 1.30 gives big gains in stellar continuum science Measuring dispersion and higher order moments when S/N=10/Å (van de Sande+ 2016)

9. Detecting winds and outflows in galaxies. Separating star formation and AGN processes and identifying shocks with ionisation mapping. Galaxy metallicities and chemical abundance mapping. Kinemetry. Scaling relations using gas rotations and dispersions. Kinematic misalignments and the origin of gas in galaxies. R (λ/δλ)>3000 in the blue and R>5000 in the red (≤1.3Å) are required to accurately constrain multi-component Gaussian fits. Emission line Science: HECTOR spectrographs Benefits of high resolution Ho et al. 2014, 2015; Medling; Groves; Davies; Hampton

10. 1.3Å resolution 3727 - 7761Å [OII] to S[II] doublet at z=0-0.15 Key cost saving is in fixed-format, replicable spectrographs. ~1200 fibres per spectrograph. Fast transmissive design by Will Saunders Refractive design by Robert Content HECTOR spectrographs ~1400mm ~1100mm

11. Conclusion HECTOR: Massively multiplexed IFU facility instrument for the AAT. Incorporates new hexabundle, spectrograph and positioning technologies, carefully matched to science requirements. First stage will be on-sky in 2018. A 50,000 galaxy survey will disentangle accretion and merger history of low redshift galaxies, to decipher their individuality.

12. HECTOR survey selection

14. HECTOR spectrographs -Science drivers Wavelength range: 3727 – 7761Å