Maunakea Spectroscopic Explorer

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1 Maunakea Spectroscopic Explorer MSE Origins and Science drivers MSE Design Project Status Andy Sheinis Director of Engineering, CFHT MSE Science Team updates

2 Canada-France-Hawaii Telescope Maunakea Spectroscopic Explorer MSE Origins and Science drivers MSE Design Project Status MSE Science Team updates New Existing

MSE Baseline Design ~4300 fiber positioner, 1.

CFHT is built like a battleship and is about as massive as Keck

Low/Mid-resolution spectrometers High-resolution spectrometers

3 MSE Baseline Design ~4300 fiber positioner, 1.5 FoV 11 m segmented primary What makes this possible? CFHT is built like a battleship and is about as massive as Keck so the pier can sustain the load of a ~10m telescope Low/Mid-resolution spectrometers High-resolution spectrometers Slow (f/4) focal ratio with a prime focus cage leads to an enclosure about the same size as Keck and Gemini

4 M 1974 Allowed to redevelop the CFHT site Keep within the same 3-D footprint must not harm the ground beyond what has already been done the less work done at the summit, the better (e.g., keep the building and pier if possible) From CFHT to MSE 1997 Redevelopment of CFHT is not a new idea e.g. SAC Working Group on the Future of CFHT (1996) Resulted in CFH 12-16m Telescope Study, Grundmann (1997) [right] CFHT 3.6m weighs 266 tons Keck is 270 tons

5 A strong heritage

6 MSE Capabilities

7 The ultimate chemical tagging experiment + Gaia follow-up Currently: 4m class spectrographs only go to ~16 mag (e.g., 4MOST, WEAVE, HERMES) Disk stars, some thick disk, and halo stars that happen to be nearby (e.g., WEAVE: only a few % halo stars)

8 The ultimate chemical tagging experiment + Gaia follow-up But Gaia will obtain proper motions for stars down to g~20 Future with MSE: Detailed chemical studies of stars across the full luminosity range of Gaia targets Studies of the outer Galaxy: the outer disk, thick disk and especially halo Spectroscopic parallaxes essential to use Gaia proper motions at faint end (where Gaia parallaxes are unreliable)

The ultimate chemical tagging experiment + Gaia follow-up Detailed chemical compositions of stars born in the same star-forming aggregates are very similar Chemical

9 The ultimate chemical tagging experiment + Gaia follow-up Detailed chemical compositions of stars born in the same star-forming aggregates are very similar Chemical tagging, especially in conjunction with Gaia astrometry, reconstructs ancient star-forming aggregates to follow the formation sequence of the Galactic disk and halo

The Dark Matter Observatory MSE will provide vast datasets of line-of-sight velocities for tracing the dark matter distribution of halo on all spatial scales Probing sub-halos around the Milky Way

10 The Dark Matter Observatory MSE will provide vast datasets of line-of-sight velocities for tracing the dark matter distribution of halo on all spatial scales Probing sub-halos around the Milky Way (via heating of cold stellar streams) Dynamics of dwarf galaxies via datasets of potentially hundreds of thousands of stars Clusters of galaxies (for Virgo, velocities of every baryonic structure brighter than r~24, including ~50000 globular clusters within the virial radius)

11 Linking galaxies to the large scale structure of the Universe Low resolution spectrograph probing galaxy evolution over all redshifts through the peak of star formation and galaxy assembly in the Universe Broad wavelength to 1.8 m to reach beyond cosmic noon

12 Time Domain Astrophysics Time domain astrophysics (TDA)! LSST followup machine Synergistic TDA ~100 observations of 5000 quasars spread over years to map the structure and kinematics of the inner parsec of supermassive black holes actively accreting during the peak quasar era (Compare with ~50 nearby, low luminosity AGN that currently have high quality measurements)

13 From Science to Capabilities Wide redshift range of interest UV to Near-IR, R~3000 mode Stellar chemical tagging R~40,000 mode Intervening absorption (IGM, CGM) / sky lines R~6000 mode Continuum flux levels accurate spectrophotometry Small velocity dispersions precise velocities High surface density of targets many close-packed fibers Many targets wide field of view Faint targets, many targets large primary aperture Faint targets great image quality, optimal fiber size & positioning Surveys ranging from few nights to 1000s of deg 2 dedicated facility to deliver science data for both legacy and PI-led surveys

14 Need for Such a Facility is Internationally Recognized In the USA, NOAO and LSST released a study of the resources needed to accomplish LSSTenabled science cases* and concluded that access to a highly multiplexed, wide-field optical multi-object spectroscopic capability on an 8m-class telescope, preferably in the Southern Hemisphere is a high priority and suggested the possibility of joining an international effort to implement a wide-field spectroscopic survey telescope like MSE or a future ESO wide-field spectroscopic facility. In Europe, the ESO Future of Multi-Object Spectroscopy Working Group Report* concluded that a large aperture (10-12m class) optical spectroscopic survey telescope could enable transformational progress in several broad areas of astrophysics, and may constitute an unmatched ESO capability for decades and recommended ESO move forward to complete a more rigorous conceptual design study and be open to considering international partnerships in all of the above.

Enclosure: Calotte style with vent modules for excellent airflow Fiber Transmission System: 3,249 fibers leading to low/moderate resolution spectrographs; 1,083 fibers leading to high resolution

15 Enclosure: Calotte style with vent modules for excellent airflow Fiber Transmission System: 3,249 fibers leading to low/moderate resolution spectrographs; 1,083 fibers leading to high resolution spectrographs Low/Moderate resolution spectrographs: located on both instrument platforms Fiber Positioner System: 4,332 positioners providing simultaneous complete full field coverage for all spectroscopic modes, with upgrade path to multiobject IFU system Wide Field Corrector and Atmospheric Dispersion Corrector: 1.5 square degree field of view Telescope Structure: prime focus configuration, high stiffen-to-mass ratio open-truss design to promote airflow M1 System: 11.25m aperture with m hexagonal segments MSE is a rebirth of the CFHT by replacing the existing 3.6m telescope facility with a Telescope and Enclosure Piers: modified CFHT structures High resolution spectrographs: located in Coude room for environmental stability SnowPAC m-class telescope equipped with a dedicated wide-field highly multiplexed fiber-fed spectroscopic facility Consider LAMOST or SDSS, on an 11m telescope, situated at arguably the best astronomical site on the planet

16 Telescope Conceptual Design Telescope structure designed by industry in Spain (ELT/ESO) heritage Significant M1 expertise and heritage in China as a result of TMT/12m

Fiber positioning system Critical subsystem; primary system in development in Australia with USTC providing development of independent back-up system, reflecting the importance of this component to

17 Fiber positioning system Critical subsystem; primary system in development in Australia with USTC providing development of independent back-up system, reflecting the importance of this component to MSE Positioners - >3,200 LMR fibres and >1,000 HR fibres with full-field coverage Metrology camera system to provide closed-loop positional feedback Overall system accuracy is 5 um (goal), to be demonstrate by lab testing

18 MSE Positioner Same technology at FMOS on Subaru and 4MOST (ESO) Very close minimum target separation, < 1mm Patrol radius > pitch, so >3-5 fold sky coverage

High Resolution Spectrograph Conceptual spectrograph designs are results of interactions between scientists and engineers given considerations for science

19 High Resolution Spectrograph Conceptual spectrograph designs are results of interactions between scientists and engineers given considerations for science motivations and the current technologies to produce large aspheric optics and large (mosaic) dispersers reliably. 1 HR spectrograph conceptual design (R=40K/20K) in development at NIAOT Potentially the highest profile science component of MSE given uniqueness of science case and timing with respect to Gaia Three different wavelength windows in optical range, with blue and green arms operating at R=40K to identify large number of chemical species at bluest wavelengths

20 Green channel R=40K/20 K F/2.05 off-axis collimator design (0.75 Red fibers) channel R=20K Blue channel R=40K Opening angle 67.5 High Resolution Spectrograph HR spectrograph conceptual design (R=40K/20K) in development at NIAOT K. Zhang Successfully passed Conceptual Design in 2017 In discussions with vendors for 2 highest technical risks: Dispersers Aspherics

21 Low / Moderate Resolution Spectrograph LMR spectrograph conceptual design (R=3000/6000, 1.0 ) provided by CRAL. Four-arm design Off-axis Schmidt f/2 collimator LR/MR change by switching dispersive elements (VPH or VPH + prism) Reasonable VPH grating demand Currently implementing the review panel s recommendations to pursue alternate optical designs for risk reduction

22 Existing surveys on small telescopes: Calipha, SAMI, Manga, Hector (planned) etc. Deployable Integral Field Units SDSS/MANGA A deployable IFU system is planned for MSE (currently baselined as a second generation capability) Critically important to develop the detailed requirements of this system and the possible technical implementation now, for integration into the overall MSE system design USTC (engineering) starting to initiation technical feasibility studies Essential that this is accompanied by a scientific feasibility study investigating major science goals, including number and size of IFUs, size of spaxels, resolution etc, in relation to other wide field IFU systems (e.g., SAMI, MANGA, etc) Is there interest in the Chinese astronomy community to lead this study (science + technical)?

23 MSE Design Review Blitz Completed last year an extensive set of CoDR level design reviews for MSE with global partners These reviews collectively informed the important Systems Design Review held in January 2018 in Waimea

Science Development 2018+ System Level CoDR Panel: Chair: Michael Strauss (Princeton) Scott Roberts (TMT) Hermine Schnetler (STFC/ATC) Ken Chambers (Hawaii)

held in January in Waimea, following a busy year that saw Conceptual Designs completed for 8 different subsystems (including HRS NIAOT; including Fiber

24 Science Development System Level CoDR Panel: Chair: Michael Strauss (Princeton) Scott Roberts (TMT) Hermine Schnetler (STFC/ATC) Ken Chambers (Hawaii) Rob Sharp (ANU) Detailed Science Case written in 2015, that informed the development of the Science Requirements in 2016 MSE Systems Conceptual Design Review held in January in Waimea, following a busy year that saw Conceptual Designs completed for 8 different subsystems (including HRS NIAOT; including Fiber Posititoning System USTC) Very useful process with excellent recommendations from the panel Prominent among these was the development of a Design Reference Survey for MSE

25 MSE is cost capped up front at US$ 313M A cost that isn t prohibitively high for ~6 partners to share but we expect will enable much of the MSE science case Concept Design phase funding from 2 sources (~50/50) CFHT direct budget In-kind contributions from all partners Total value of construction proposal ~US$ 10M MSE Contributions Contributions During Conceptual Design Phase India, $143,940 2% Spain, $711,278 9% Hawaii, $662,034 9% France, $2,494,499 32% Australia, $157,060 2% Canada, $2,427,017 32% China, $1,108,437 14%

Current schedule and costings DRS1 released New call for Science Team

France, US MSE managed as a cost-capped project (USD313M, 2018 economics) No

design MSE subsystems as required by SRD Current costing of MSE based on

26 Current schedule and costings DRS1 released New call for Science Team membership, leading to DRS Decadal planning decisions: Australia, Canada, France, US MSE managed as a cost-capped project (USD313M, 2018 economics) No cost constraints imposed during Conceptual Design Phase; partners asked to design MSE subsystems as required by SRD Current costing of MSE based on Conceptual Design studies is ~USD370M Rationalization of cost/scope/science in 2018/2019

The MSE Collaboration Organizationally, MSE is: One of the Maunakea

empowered by the CFHT Board to perform the role of MSE Board: All MSE

NOAO (USA) and Texas A&M asked to join as observers.

partners indicating expected contributions to PDP (total cost of PDP

27 The MSE Collaboration Organizationally, MSE is: One of the Maunakea Observatories, A project of the Canada France Hawaii Telescope Corporation to upgrade to an 11.25m dedicated spectroscopic facility The MSE Management Group (MG) is empowered by the CFHT Board to perform the role of MSE Board: All MSE partners - currently Australia, Canada, China, France, Hawaii, and India - have equal status (i.e., it is an international project, not a C-F-H project) NOAO (USA) and Texas A&M asked to join as observers. MoU in negotiation for oversight of the Preliminary Design Phase, with partners indicating expected contributions to PDP (total cost of PDP ~USD25M) Separate agreement to be negotiated to manage MSE in construction/operations phase (i.e., post-pdp) MSE Science Advisory Group (SAG) is appointed by the MG and is consulted by the MG on all aspects of science development

MSE-China Suijian Xue (NAOC) Xuefei Gong (NIAOT) Gongbo Zhao (NAOC) Yingjie Peng

It is one of the original partners in the project During the Conceptual Design, China was

Fiber Positioning System Chinese astronomers were ~10% of the science team of MSE and took

galaxy clusters, evolution and cosmology Tremendous opportunity for China and Chinese

including the high resolution spectrograph, IFU system, M1 system - during the forthcoming

28 MSE-China Suijian Xue (NAOC) Xuefei Gong (NIAOT) Gongbo Zhao (NAOC) Yingjie Peng (Peking/KIAA China has been a member of MSE since the start of the Project Office in It is one of the original partners in the project During the Conceptual Design, China was the lead developer of the High Resolution Spectrograph and a major contributor to the Fiber Positioning System Chinese astronomers were ~10% of the science team of MSE and took a prominent role in the development of the extragalactic science cases, including AGN, galaxy clusters, evolution and cosmology Tremendous opportunity for China and Chinese Institutes to take very prominent role in both science and engineering developments including the high resolution spectrograph, IFU system, M1 system - during the forthcoming preliminary design phase Now is the time to increase the scientific involvement of the Chinese astronomy community to

Science Development 2018+ See http://mse.cfht/hawaii.

29 Science Development See New call for science team members in March 2018, ongoing, that has resulted in the science team nearly doubling in size

Thank you! For more information: http://mse.cfht.hawaii.

30 Thank you! For more information: To join the Science Team, please contact the Project Scientist or your SAG representatives

Science and Status of the Maunakea Spectroscopic Explorer

Science and Status of the Maunakea Spectroscopic Explorer Science and status of the Alan McConnachie MSE Project Scientist CFHT Users Meeting, May 3 2016 Maunakea Spectroscopic Explorer Alan McConnachie