maunakea spectroscopic explorer -...

Andy Sheinis

Director of Engineering, CFHT

Maunakea

Spectroscopic Explorer

MSE Origins and Science drivers

MSE Design

Project Status

MSE Science Team updates

Existing

New

Canada-France-Hawaii TelescopeMaunakea Spectroscopic Explorer

Maunakea

Spectroscopic Explorer

MSE Origins and Science drivers

MSE Design

Project Status

MSE Science Team updates

Maunakea Spectroscopic ExplorerMSE Baseline Design

~4300 fiber positioner, 1.5°FoV

Low/Mid-resolution spectrometers

High-resolution spectrometers

11 m segmented primaryWhat 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

Slow (f/4) focal ratio with a prime focus cage leads to an enclosure about the same size as Keck and Gemini

Maunakea Spectroscopic ExplorerFrom CFHT to MSE

1974MAllowed to redevelop the CFHT siteKeep within the same 3-D footprintmust 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)

Redevelopment of CFHT is not a new ideae.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 tonsKeck is 270 tons

1997

Maunakea Spectroscopic Explorer

A strong heritage…

Maunakea Spectroscopic ExplorerMSE Capabilities


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)


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 tagging, especially in conjunction with Gaia astrometry, reconstructs ancient star-forming aggregates to follow the formation sequence of the Galactic disk and halo

Maunakea Spectroscopic ExplorerThe 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)


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 1.8m to

reach beyond cosmic noon


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)


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 deg2 → dedicated

facility to deliver science data for both legacy and PI-led surveys


Need for Such a Facility is Internationally Recognized

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.”

In the USA, NOAO and LSST released a study of the resources needed to accomplish LSST-enabled 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”.


SnowPAC - 20180312

Enclosure: Calotte style with vent modules for excellent airflow

Telescope and Enclosure Piers: modified CFHT structures

Fiber Positioner System: 4,332 positioners providing simultaneous complete full field coverage for all spectroscopic modes, with upgrade path to multi-object IFU system

Wide Field Corrector and Atmospheric Dispersion Corrector: 1.5 square degree field of view

Fiber Transmission System: 3,249 fibers leading to low/moderate resolution spectrographs; 1,083 fibers leading to high resolution spectrographs

High resolution spectrographs: located in Coude room for environmental stability

Low/Moderate resolution spectrographs: located on both instrument platforms

Telescope Structure: prime focus configuration, high stiffen-to-mass ratio open-truss design to promote airflow

M1 System: 11.25m aperture with 60 1.44m hexagonal segments

MSE is a rebirth of the CFHT by

replacing the existing 3.6m

telescope facility with a

11m-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

Maunakea Spectroscopic ExplorerTelescope 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

Maunakea Spectroscopic ExplorerFiber 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

Maunakea Spectroscopic ExplorerMSE 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

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

1

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.


High Resolution Spectrograph

2018-5-1120

Green channel

R=40K/20K

Blue channelR=40K

Red channelR=20K

F/2.05 off-axis collimator design (0.75” fibers)

Opening angle67.5°

HR spectrograph conceptual design (R=40K/20K) in development at NIAOTK. Zhang

Successfully passed Conceptual Design in 2017

In discussions with vendors for 2 highest technical risks:

DispersersAspherics


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 implementingthe review panel’s recommendations to pursue alternate optical designs for risk reduction

Maunakea Spectroscopic ExplorerDeployable Integral Field Units

• Existing surveys on small telescopes: Calipha, SAMI, Manga, Hector (planned) etc.

• 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) ?

SDSS/MANGA

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

MSE Design Review BlitzMaunakea Spectroscopic Explorer

Maunakea Spectroscopic ExplorerScience Development 2018+

¯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

• System Level CoDR Panel:

• Chair: Michael Strauss (Princeton)

• Scott Roberts (TMT)

• Hermine Schnetler (STFC/ATC)

• Ken Chambers (Hawaii)

• Rob Sharp (ANU)

Maunakea Spectroscopic ExplorerMSE Contributions

Contributions During Conceptual Design Phase

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

Australia, $157,060

2%

Canada, $2,427,017

32%

China, $1,108,437

14%

France, $2,494,499

32%

Hawaii, $662,034

9%

India, $143,940

2% Spain, $711,278

9%

Maunakea Spectroscopic ExplorerCurrent schedule and costings

DRS1 released

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

New call for Science Team

membership, leading to DRS

• Current costing of MSE based on

Conceptual Design studies is ~USD370M

• Rationalization of cost/scope/science in

2018/2019

Maunakea Spectroscopic ExplorerThe 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

Maunakea Spectroscopic ExplorerMSE-China

Gongbo Zhao (NAOC) Yingjie Peng (Peking/KIAA)Suijian Xue (NAOC) Xuefei Gong (NIAOT)

• China has been a member of MSE since the start of the Project Office in 2014. 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 continue to shape MSE and have a leadership role in the collaboration

Maunakea Spectroscopic ExplorerScience Development 2018+

See http://mse.cfht/hawaii.edu/sciteam

New call for science team members in March 2018, ongoing, that has resulted in

the science team nearly doubling in size

http://mse.cfht/hawaii.edu/sciteam


• For more information:

• http://mse.cfht.hawaii.edu

Thank you!

• To join the Science Team, please contact the Project Scientist or your SAG

representatives

• [email protected]

https://arxiv.org/abs/1606.00043

https://arxiv.org/abs/1606.00043

maunakea spectroscopic explorer -...

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