PoS(MULTIF2017)082 https://pos.sissa.it/ ] which was compiled by members of the TMT 1 ∗ [email protected] Reporting aspects of the 2015 TMT Detailed Science Case [ The Thirty Meter Telescope (TMT) will providesources exciting of capabilities many for different the types. study of Future high ground(ELTs) energy based have general important purpose roles extremely large to telescopes tron play stars, in super studies novae of andfeedback low gamma-ray and mass bursts other X-ray (GRBs), processes binaries super-massive in black their (LMXBs)perspective host holes and of galaxies, (SMBH) TMT, neu- colliding I and galaxies describe and a darkthat matter. selection the TMT From of (and the possible the studies other that futureresolved ELTs) will and will cadence illustrate provide observations such the and as capabilities the support for importancecilities. ToO of observations, I coordinated time observations give with an other overview fa- ofselection and the development timeline process for for the new beginning instruments. of TMT operations and the flexible ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). International Science Teams, Science Advisory Committee and others. XII Multifrequency Behaviour of High Energy12-17 Cosmic June, Sources 2017 Workshop Palermo, Italy Warren Skidmore Thirty Meter Telescope International Observatory, 100CA West Walnut 91105, Street, USA Suite 300, Pasadena, E-mail: The possibilities for comprehensive studies involving the Thirty Meter Telescope ofhigh the energy ’zoo’ sources. of PoS(MULTIF2017)082 - γ 1 m pixel scale. Instruments have fixed gravity vector by being located on the Nasmyth µ An overview of the design for the Thirty Meter Telescope Observatory. The Ritchey-Chrétien The TMT Observatory is being designed to support both queue scheduled and classical (i.e. The Thirty Meter Telescope (TMT) is one of three general purpose extremely large ground The ELTs form part of the suite of facilities that will be available for astronomers in the future, astronomers directly involved) observing modes.large A cross mix partner of key small programs will programswill be for be carried individual provided out. PIs so Remote and that operations principaldata and investigators eavesdropping by (PIs) modes observatory can staff participate without in traveling or to monitor the the observatory. gathering Flexible of scheduling will be used to design has an effective0.46 f/15 milli-arcsends/ final focalplatforms ratio and with any a instrument can 20"system be can field selected feed by of up rotating to view, thebe 3 2.62m accommodated tertiary instruments on diameter mirror. and the up focal The Nasmyth to first platforms. plane about light (Credit: 10 with adaptive TMT instruments optics International (depending Observatory) on instrument choices) can Figure 1: based telescopes (ELTs) planned totremely begin Large operations Telescope (E-ELT) in and the 24.5/22min mid-2020s. Chile. Giant The Magellan TMT The Telescope will are 39m beat being European constructed Observatorio constructed in Ex- del the Roque northern de hemisphere, eitherlate los on 2020s. Muchachos, Maunakea, La Hawaii Palma or and operations are planned to startproviding in a the range of key capabilities alongside wide angle survey telescopes, radio, X-ray and Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources 1. Introduction to TMT ray telescopes and gravitational wavebridges observatories. between astrophysics Exciting to high-energy possibilities and exist particle for physics. research that PoS(MULTIF2017)082 α 5000. ∼ ), correlating 2 . Determining a forest will allow 3 α 2 Ground based experiments searching for the interaction of dark matter particles with baryonic The characteristics of the dark matter halo are determined using gravitationally lensed back- The TMT International Observatory partnership presently consists of India, Canada, Japan, The large increase in sensitivity provided by TMT will allow the measurement of the Lyman- On a more fundamental level, determining the high spatial frequency fluctuations in the bary- Dark energy is driving the acceleration of the expansion of the universe. A major problem matter have so far beenmatter unsuccessful. particles themselves Astrophysical to studiesmatter allow be halos the examined in interactions clusters by between of studying interacting dark the galaxies. the structure andground dynamics tracers of and dynamical dark studies of stellar and gaseous sources, see Figure these with redshift. This technique will bebackground more measurements. successful when combined The with cosmic redshifts microwave dynamics to (and the hence lensed the gravitational quasars mass)using and and diffraction super redshift limited novae of high the and spatial gravitational resolution the lens spectroscopy internal will with be spectral obtained resolution of R 2.3 Dark Matter self-interaction cross-section China, the University of California andsubsystems Caltech. within Each the partner is observatory. responsibleconstruction for At or delivering the in various the time final ofdelivering design an writing, phase operational all and observatory development critical in is the sub latter proceeding systems part in of are all the areas either 2020s. necessary in for 2. Science areas in which TMT is envisioned to2.1 make contributions Baryonic Power Spectrum on the Smallest Scales onic power spectrum, quantifying deviationsmuch in smaller the than probed power by spectruminflation. Planck, from will unity provide on important spatial information scales on the fields that2.2 drove Studying Dark Energy with Time-delay Cosmography facing modern cosmology is distinguishing betweenent different possible dark dark energy energy models models. have Differ- differentthe equations equation of state of but state theremeasure and is both always the the a cosmic time degeneracy curvature between delays andally parameter. lensed the quasars angular To and separations break supernovae using between this high multiple spatial degeneracy images resolution we of imaging (see gravitation- need Figure to Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources optimize science output based on thein atmospheric the conditions queue. and priorities of observing programs forest with a much greatertinuum density sources of then about sight 200x lines. greaterachieved spatial By density with using will quasars. faint be achieved background compared Significantly galaxiesmuch to more as improved that stringent presently the measurements constraints con- of to thethe be ratio placed Lyman- with on the the observed ratio Baryon of fraction. cold to hot dark matter and reconcile PoS(MULTIF2017)082 ]). 2 3 N

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0 0 .5 Figure 3: Right: The mass density2015, of [ the cluster derived using lensed image positions (Figures from Massey et al., Figure 2: an early type galaxy cluster (Figure from Kelly et al, 2015, [ Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources PoS(MULTIF2017)082 to 7 and probe the structure of BLR . Present telescopes cannot pro- ) to obtain high spatial resolution 3 3.1.1.1 4 30", see Figure ≥ 0.5 spans ∼ formed early in the history of the universe, within the first billion years. Us-

M 10 . By collecting many measurements we can trace the growth history of typical 10 bh A few bright quasars are observed at redshifts of z>6, this tells us that black holes with masses In the local universe we can carry out near-IR IFU observations of all types of nearby galactic One source of the initial seed black holes in the early universe could be from massive stars. The SMBH sphere of influence can be resolved in diffraction limited observations with TMT We will be able to constrain the size of the broad-line region, R Galaxy clusters act as strong gravitational lenses. Many of the strong lensing arcs of back- solar mass SMBHs at high-redshifts in moderate or low luminosity AGNs. 8 of about 10 centers to investigate howgalaxies SMBHs are fueled and how they control theSpectroscopy of evolution galaxies of at their redshifts(IMF, host z>2 i.e. will the let range us ofheavy investigate stellar whether IMF masses) the at evolves initial over higher mass cosmic redshiftcould function time. grow could to Importantly, provide form evidence quasars. a for source a top- of intermediate mass seed2.5.2 black Central holes regions, Dusty that Torus and Black Hole Mass and the bright centraltroscopy AGN with point R<4000 source inresolution isolated. the to near-infrared allow Diffraction with stellar-dynamical limitedholes, the analysis spatially M that TMT resolved yields of spec- the many mass AGN of will the have central the massive spatial black vide the required fidelity of observations,needed the to sensitivity measure and the spatial redshifts resolution of provided thein by arcs the TMT and density is to profile detect of substructure the in lensing the cluster. arcs due to substructure 2.5 Active Galaxies and Black Hole Growth 2.5.1 Seeds for Super Massive Black Holes spectroscopy of quasars at z>6ulations we will and be that able from to ’super-Eddington’the differentiate accreting metal between abundances, intermediate the gas black light kinematics from and holes outflowsunderstand stellar (IMBH). in fueling, pop- the Measuring accretion quasar rates host and galaxies the will formation help of us massive to black better holes at early times. 10 the accretion disk region using thedelays technique of of the reverberation response mapping. of This broad technique emission uses lines time- to continuum variations and requires rapid optical ing an integral field spectrograph unit (IFU) (see Section ground galaxies have widths belowquired 0.1" to and resolve therefore and adaptive separate opticstypical them (AO) clusters from based the at imaging background redshifts is sky. of re- The z strongly lensed region around Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources full inventory that includes very faint clustergrams members including has X-ray been observations a of limitation so thematerials. far. hot Synergistic gas pro- will help to complete the inventory of baryonic 2.4 Cosmology from clusters of Galaxies PoS(MULTIF2017)082 1s to 3s. ∼ 0.5-2. ∼ 5 10mins. Such short sampling times are beyond the reach of ∼ , the structure of the accretion disk and broad-line region and can samp 2.5.2 0.5-2 can be observed using near-IR IFU spectroscopy. Synergistic observations with ∼ . Dual AGN systems may be buried inside the obscuring dusty structure and NIR (1- 0.5 or 5 Gyr. Further synergistic observations with ALMA will probe the outermost (cold) 4 ∼ m) polarimetric imaging with TMT will be needed to reveal the conical centrosymmetric In the hierarchical model of galaxy evolution, a large fraction of elliptical galaxies are expected The outflows induced by AGN winds and jets that prevent runaway star formation in massive AGN may have a ’clumpy’ dust torus whose properties are strongly affected by AGN activity Blazars are a sub-class of Quasars or AGN whose emitted jets happen to point toward Earth. To explore the acceleration mechanism we will need simultaneous observations of a Blazar As described Section µ 2.5 to have stalled binarynearest black elliptical holes as galaxies a willand result be their of brought presence galaxy together should mergers.around be due 1pc evident to Non-active they from binary dynamical are stellar BHs friction expectedbe motions. in to with able stall the Once nearby due to the stars to resolve BHs lowFigure the stellar reach densities. expected a separation stalling TMT of with radii adaptive of optics binary will BHspolarization pattern and centered reveal on each active AGN. dual nuclei, see be mapped with greatobservable accuracy with TMT. and images of the jet morphology2.6 obtained Binary in Super-Massive Black all Holes wavelengths ALMA of molecular outflows andare with needed the to VLA give a of complete synchrotron picture emission of from AGN feedback jets at and redshifts outflows of z galaxies at z and the availability of fuel for thetions AGN. with Mid-IR the high 30m spatial resolution TMT diffraction willup limited be to observa- z able to resolve theregions dust of torus the in torus the structure. centergions of High where galaxies spatial at the resolution redshifts effects NIR polarimetric ofused imaging magnetic to will fields minimize show effect the the are re- study dilution strongest. of of the Polarimetric the evolution and observations polarized morphology can AGN of be the flux material by obscuring the host2.5.3 AGN galaxy core. Blazars starlight and allow the Particles in those jetsbe are by accelerated shock to waves, relativistic turbulence,depends energies. and/or strongly magnetic on The reconnection, magnetic acceleration thevariable field efficiency mechanism linear of geometry. polarization may each on time Also, mechanism scales each down to mechanism a will few minutes. showwith different TMT time- and the Cherenkhov Telescopeolution Array optical (CTA). and TMT mid-IR will spectra be of usedneous nearby to AGN observations gather on will moderate timescales let res- of us a relateenergy few the minutes electrons. or magnetic less. field Models direction Simulta- of to the<30s the acceleration at acceleration mechanisms wavelengths of observable predict the with highest- micro-variabilityresolution the on wide TMT. timescales wavelength A coverage spectro-photometry full with investigation sampling requires times optical of and NIR low Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources and mid-IR observations with t existing telescopes. PoS(MULTIF2017)082 - γ 500) ∼ K blackbody radiation 5 m spectroscopy (R µ relation or maser disk kinematics) will σ 2000) and 1-2.4 ∼ 6 (such as from the M- ]). bh 4 Top left: Original JVLA image of galaxy 2MASXJ1203. Top center right: Model of the galaxy The suggested fire ball model for Gamma Ray Bursts (GRBs) is an inhomgenous relativistic A Tidal Disruption Event (TDE) occurs when a star makes a close approach to an SMBH and TDEs will be visible by TMT to z>6, less than 1Gyr after the Big Bang, enabling constraints outflow with inverse Compton or synchrotron emission, internal velocity variations that cause provide a better calibration of the models for TDEs. 2.8 Gamma Ray Bursts 2.8.1 The Explosion is ripped apart by tidal forces.in TDEs optically provide ’normal’ a galaxies, means i.e. tomaterial measure forms galaxies the an that mass accretion and do disk spin around not of the show black SMBH. AGN Soft holes activity. X-ray and The UV disrupted 10 stellar on SMBH properties and evolution over aindependent vast measurements range of of cosmic M time. TDEs in nearby galaxies with Figure 4: image profile assuming aterm simple elliptical (right). galaxy profile Lower(Figure (center) center from and and Rubinur with et right: al., the 2017, Residual addition [ after of an subtracting exponential of the2.7 model profiles Tidal reveals Disruption Events two cores from the inner ofradiation. the accretion Many disk TDEs isTelecope will reprocessed (LSST) be from and found the followup intimes inner observations large-area with accretion will TMT surveys region require of such <1hr into Target as forthat of optical optical is the Opportunity simultaneous spectroscopy Large with (R (ToO) CTA. response Synoptic Survey Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources PoS(MULTIF2017)082 m) µ 100) in the optical to NIR (400nm to 2.2 ∼ 7 1 day of any kilonova event associated with short GRBs. ≤ 6 is limited by a lack of sufficiently bright GRBs but with TMT’s large  1 day and continue for up to 30 days after the GRB. ∼ Observations of the optical counterparts for short GRBs limit any accompanying supernova- GRBs can serve as a background source whose light is affected by absorption as it passes GRBs can be used to trace early galaxy and star formation that re-ionized the universe as Optical spectroscopy with TMT of low redshift GRBs will identify any faint associated super To track the rapid changes in the flux from the fireball, the light gathering power of TMT is There are two forms of GRBs that are observed and different ideas for the cause of GRBs of The idea of collapsing massive stars forming long GRBs has some observational support be- like event to being >50be times consistent fainter with than an normalthe r-process form SNe powered of Ia kilonova. short or GRB To hypernovaeperform progenitors, ToO improve Ic. observations TMT the in with However observational a they constraints NIR may AO on fed IFU will be the ideal instrument to through cool and/or neutral hydrogencentral gas regions clouds of along the theabout host line galaxies, the of in chemical sight the enrichment butoccurs. vicinity located history of in This of the the contrasts galaxies dense GRB. withlow directly This the density in regions yields use where the critical of materials region information quasars have been as where affected background by the gas targets enrichment injection, whose infallGRBs lines-of-sight and can mixing. probe be detected withPresently, TMT progress at at greater z distances than the farthest quasars and early galaxies. novae. At this time, all confirmedstars. long GRB The host host galaxies have galaxiesgalaxies, been implying also found an have to age be a for actively the low forming progenitors total of stellar long GRBs mass of and <0.2 are Gyr. bluer than present-day spiral 2.8.3 Probes of High Redshift Inter-Galactic Medium and Inter-Stellar Medium needed to provide low resolution spectroscopy (R each form. The rarer short GRBs,The that majority last long <2s, are GRBs, thought that to(an last be important between the tracer result 2 of of to massive neutron star 1000s, star formation are mergers. at thought high to z). be collapsingcause massive some, stars but notredshifts all, of z>0.5 long to GRBs 1,and any at followed super low with nova component a redshifts, will telescope z<0.5, beto as start so large exhibit within faint as super f that TMT they feeding nova can a behavior. only NIR be AO For identified fed IFU. Followup would need aperture and fast response time fornear-IR ToO spectra observations we of will faint be GRBs able outlie to at to obtain near-IR very high wavelengths. high signal redshifts, to z>7, noise where the relevant spectral features Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources ray emission and mild internal shocksa at factor larger radii 10 that over cause 1 opticalprompt minute emission. observations, need Flux beginning variations to within of be a sampled.based few facilities. hundred Consequently, seconds The studies combined of of telescope the and the trigger instrument GRB detection response fireball from time require space needs to be <10 minutes. with the required rapid 1s sampling.need To 100s investigate asymmetries exposure in time the high shape signal of to the noise fireball spectro-polarimetric we measurements. will 2.8.2 Progenitors PoS(MULTIF2017)082 through the varied galaxy types in

50ms) of systems that exhibit eclipses. 1 M ∼  samp 8 . 5 to brown dwarfs of

100 M ∼ 4000) with a high sampling rate (T ∼ Left: A three color image of the current capabilities using HST ACS (F814W) and WFC3 (F110W, Stellar population studies with TMT will use a variety of AO fed diffraction limited near- and Matter transfer from the Roche lobe filling secondary star toward the heavier compact primary The spatial resolution and sensitivity of the TMT will enable studies of individually resolved With the TMT, about 100 eclipsing systems can be studied with high signal to noise, representing Figure 5: F160W), the limit of the spatialon resolution that our can current be achieved knowledge atinstrument this of IRIS time. with this Right: the region, A NFIRAOS simulated AO. as image (Credit: based observed Tuan Do, with UCLA) the Z, J, and Kmid-IR band IFUs, using high TMT’s resolution first spectrometers and light complementary high observations contrast with exAO similar systems. spatial ALMA resolution,of will penetrating dust-enshrouded provide the star-forming regions. dust to probe the core 2.10 Cataclysmic Variables and Novae (white dwarf) in Cataclysmic Variables (CVs) andor similar Black types Hole of primaries, systems (some some have have neutron whitethe star dwarf compact secondaries) often primary. forms an The accretionof emission disk particular around from interest CV is accretion themechanism disks variable for converting flickering can gravitational component energy be to that mapped radiationtransport provides and and out the important characterized, mechanism from clues for the about angular disk. moment the yet This mechanism it for is angular perhaps momentum thewould transfer is form. most poorly important To understood map astrophysical the process,servations flickering without (R in which CV no accretion disks compact requires structures optical spectrophotometric ob- stars in star forming regionsstudy throughout the the stellar local populations group andrange of determine of galaxies the masses, and initial from beyond. stellar mass This function will (IMF) let over us the entire Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources 2.9 Pre-Main-Sequence and Main-Sequence Stars the local group. Presentresolution studies of are exiting restricted facilities, see to Figure within the Milky Way due to the limited spatial PoS(MULTIF2017)082 10,000 km/s) ∼ 5000 - 30,000) to characterize the ∼ 9 Novae are CV type systems that undergo periodic nuclear burning of the material accreted by Observations suggest that high-velocity (HV) SNe Ia (V(SiII) > 12,000 km/s) likely originate Testing for redshift evolution of SNe Ia requires the TMT because better spectroscopic clas- To carry out high precision cosmology using SNe Ia requires deciding between the single vs. To identify the SNe Ia explosion mechanism and test for differences in the early ejecta com- the white dwarf primary. Novaesical timescales novae). range Novae from have years polar-blob, (recurrent equatorial-ringtions geometry novae) in and/or to their multiple millennia ejecta blob (clas- like shells. condensa- process The on non-spherical the Nova compact ejecta star shell surface geometryat is means not the that symmetric. time the Important of explosive aspects outburst ofburning the and process ejecta the activity on occur early the forming whitewith fireball dwarf diffraction shell limited surface. provides adaptive important optics, Because information outburstingobjects of novae on one within the week the a after excellent outburst, few spatial the kpc physics resolutionIR will occurring become of IFU. within extended TMT the TMT fireball will can need beoptical to probed to with carry mid-IR a spectrophotometry out near- and Target spectropolarimetry of (R Opportunity (ToO) observing programs that gather Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources a range of mass transfer rateswith and existing telescopes. accretion disk behaviors. Such observations cannot be obtained in the inner regions of higher-luminositysubstantial galaxies from chemical metal-rich progenitors evolution that whereas have undergone normal-velocity (NV) SNe Ia (V(SiII) sification at high redshift isobtain needed high-quality spectra than for can SNe presently IaTMT be below z will obtained. = easily 1.5 10m obtain however class AO spectralimited assisted facilities with near-IR AO can spectroscopy fed better on only near-IR wavelength IFU coverage observationsand of will provide SNe spatially information up such resolve to as the the components z star of = formation the 4. rate host (SFR) galaxy Diffraction in2.11.2 the host Unveiling The galaxy. Explosion Mechanism of Type Ia Supernovae double degenerate explosion mechanism, i.e. betweenstar a white versus dwarf accreting accreting from main from sequence metals another in the white outermost dwarf. ejecta thatouter create most Each different layers spectral mechanism of signatures. the creates Observations ejecta tell different in us NV amounts that and the of HV SNe Iaposition are we chemically need different. to obtain early-phaseSNe near-IR Ia. spectra of Observations C and needcadence Mg to features of begin in a within a few sample 2 of minutes.explosion days high-z will of Also, be the a late-time beginning strong opticaloriginal of diagnostic explosion. and the of near-IR explosion the spectroscopy, and ejecta 1-2 have kinematics years a and after thermonuclear the products of the asymmetry and follow the fireballs evolution. 2.11 Supernovae 2.11.1 Characterizing high-z SNe Ia: Towards a Better Standard Candle appear to originate in lesscrease luminous with lower increasing metallicity redshift galaxies. dueprocessing. Metal-enriched to There environments the may de- creation be of an heavier evolution of elements the being ratio dependent of on HV stellar to NV SNe Ia with redshift. PoS(MULTIF2017)082 500) of shock ∼ 0.1 mag/hr at z = 2 with ∼ . Two of the instruments (IRIS and 1 ], that was compiled from the input of the 1 10 A capability that is of particular interest to astronomers interested in many high energy sources Three versatile instruments were chosen as the first light instruments in addition to a facility In core-collapse SNe, as a result of the collapse of the core, a shock wave propagates outward, The design of entire observatory has been developed to provide the capabilities to carry out 10 Myr). Shock breakouts at z>2.5 will be detectable in 8m wide angle surveys such as with ≤ WFOS) and the AO systemcopy are of actively an being existing developed, instrumentIRMS the will and third be will fed instrument, by be IRMS, the developed is AO system, closer a WFOS to close is the a seeing time limited of optical first instrument. light. IRIS and and processes is the requirementwithin for 10 the minutes TMT using observatory any tolenging instrument be requirements in able on any to the part begin of telescope takinga the structure science different sky. (for data instrument), slewing), This the the rapid adaptive optics tertiary responseoptimize system mirror imposes LGS and chal- positions (for laser and changing guide close to star thethe (LGS) correction necessary system loops) (to and configuration). initialize, the instruments Theconsidered (to operational initialize as procedures and the to set details to support of rapidrapid the response ToO TMT requirements programs operations of will plan the be three are current developed. ELT projects. TMT3.1.1 has the First most Light Instruments stringent near-IR adaptive optics (AO) system, (NFIRAOS) see Table TMT International Science Development Teamsdesign (ISDTs), of the is observatory broad to be andhigh flexible ambitious quality and optics, able and agility to forces and support large the many instrumentinstruments observing platforms that modes. of can Because the be telescope of supported itself, the is the relatively types unconstrained. of future emerging from the star asThe shock a breakout sudden has fireball, asupernova the longer radius. duration brightest and part redder Durations of color rangeX-ray a for to from supernova, a UV. a Breakouts progenitor ’shock can few star breakout’. be with seconds detectedstar a at to formation z larger 1 rate > pre- 1 because day and the and( can massive used emission stars as peaks a that in means succumb to theLSST to probe and soft the core Subaru high collapse HSC. redshift have The very expected decline short of lives a core collapse SNe is a broad range of science.that It we is cannot recognized yet thatnot imagine the yet and observatory conceived. will the The be telescope TMT used will Detailed for need Science science to Case programs [ host future instruments that we have Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources 2.11.3 Identifying The Shock Breakout of Core-Collapse Supernovae a quasi-black body spectrum and sobreakouts rapid with (< TMT 1 with night) 1-2 ToOcadence optical hr spectroscopy observations sampling (R (4 are to neededmetal 8hr) to lines for give gradually the the become temperature next prominent. evolution.pre-supernova 2 This radius, to Slower will CSM structure provide 3 and clues days mass about lossoccurred. will the at show the progenitor last such the stage as spectral of the the evolution evolution before as the the SNe 3. Summary of the Project Timeline and Planned3.1 Capabilities Science drives the design PoS(MULTIF2017)082 m µ 100 4660 ≤ 50000 @0.75" slit @0.16" slit 2000 - 10000 5000-100000 20000-100000 5-100 imaging 4000-8000 IFU Spectral resolution 1000-5000 (>7500) ]. Goals for capabilities 5 . 7 an imaging channel covering 1) ) and increased sensitivity due to being 8 The present concept for a near InfraRed 20x3" IFUs 0.05" inner 33" imaging 10" imaging 3" slit length 2" slit length 5" slit length ∼ 0.5 - 2.25" IFU >40 sq arc min (>100) Total slit length >500" over >5’ diameter field 1" outer working angle Field of view/Slit length length, 46 deployable slits 11 2’ field, up to 120" total slit m) µ ( 1 - 5 8 - 18 (1 - 5) 1 - 2.5 λ 0.8 - 2.5 0.8 - 2.5 (4.5 - 28) 0.31 - 1.1 0.31 - 1.0 0.95-2.45 , has two parallel instrument channels, an integral field spectrograph (IFS) that provides 4 plate scales and 4 corre- 6 2) Instrument Instrument - PFI First light (above double line) and potential future generation instruments [ Planet Formation InfraRed Multislit Spectrometer - IRIS InfraRed Imager and Spectrometer - IRMS Spectrometer - HROS spectrometer - NIRES spectrometer - MIRES Deployable, multi-IFU, Mid-IR AO-fed Echelle Near-IR AO-fed echelle IRMS will provide up to 46 spectra over a 2 arc minute field with a resolution of about 5000 The IRIS instrument will consist of an imager housed in the upper half of the dewar and the IRIS, see Figure High-Resolution Optical Wide-field Optical imager and spectrometer - WFOS near-IR spectrometer - IRMOS fed by the NFIRAOS adaptive optics system. Multi-object Spectrograph (IRMS) is based onthe Keck the Observatory design and of is the conceived as existingnical a MOSFIRE risk way instrument to on at provide a this shorter capabilityfield at timescale spectrographs low than cost and and developing multi-object low an tech- adaptive instrumentthe optics. use with of The multiple a power deployable reconfigurable of cryogenic integral slit the mask IRMS (see design Figure comes from 3.1.1.2 Infrared Multi-object Spectrometer - IRMS IFS in the lowerfed part. from the The first-light adaptive imager optics(NFIRAOS). is The system instrument being the is Narrow developed attached Field in beneath InfraRed NFIRAOS, Japan, Adaptive see Optics Figure the System IFS in California. IRIS is Table 1: 34"x34" using four 4k bydiffraction 4k limit Hawaii and 4RG detectors withsponding 0.004"/pixel, fields of nyquist view. sampling The IFS the has 1 2and pixel scales 1.01"x1.15"@0.009"/pixel) provided using and a lenslet two array2.25"x4.4"@0.05"/pixel). (0.45"x0.51"@0.004/pixel using an image slicer (1.13"x2.20"@0.025"/pixel and 3.1.1.1 Infra-Red Imaging Spectrometer - IRIS Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources are in parentheses.priorities Types and of needs of instruments the not TMT user listed community. here may be developed in response to the scientific PoS(MULTIF2017)082 12 Left: View of the inner parts of IRIS, the IFS in the lower half of the dewar, the imager in the Representation of the focal plane in the IRIS instrument. The four Hawaii 4RG (green squares) Figure 7: upper half, the ’snout’ that containsThe the large blue OIWFS box and is the NFIRAOS mounting andinstrument struts IRIS platform. is to (From: seen the J. below bottom Larkin, with of the UCLA) NFIRAOS. donut Right: shaped cable wrap on the floor of the Figure 6: create a diffraction limited imagerrepresented covering by 34"x34" the with small 0.004" coloredsensors pixels. rectangles (OIWFS) in The are the fields shown. center. of(Credit: view The The J. of patrol Larkin, yellow the fields UCLA) circle IFS of shows are the the on-instrument full wavefront field of view of the first light AO system. Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources PoS(MULTIF2017)082 ). The beginning of the process 10 A multi-object wide field optical spectro- 13 ) and provides spectral resolution up to 8000, >40 sq. arc min field 9 m with a sensitivity of about 3.3 magnitudes more in J and K compared µ m. Programs would trade off the wavelength coverage, number of targets and m to 2.45 µ µ Left: IRMS as installed at the upper port of the NFIRAOS adaptive optics system (From: B. types m to 1.1 In order to ensure that new capabilities arrive at the observatory every two to three years, an The planned construction timescale for the TMT is approximately 10 years and the develop- The MOBIE (Multi-Object Broadband Imaging Echellette) design for WFOS was developed µ of view, multiplexing capabilities from0.31 a single target up to 200 and wavelength coverage from instrument development process has been established (see Figure resolution. The system would also work as an optical imaging camera. 3.1.2 Development plans for 2nd generation instruments and existing ideas for instrument ment timescale of a facility classfor instrument for proposed TMT 2nd is generation about instrument the studies same. was Consequently released the in first September call 2017. is based on community explorationscapabilities that of identify the the TMT scientific userand priorities down community. selection and followed Subsequent required by a stages instrument standard instrument involvethere development initial process. is technical The no process exploration is predefined flexible, scientific instrument interests delivery of the sequence, TMT the user community. process can respond to changes in the covering 0.97 Figure 8: Mobasher, UCR). Center: The reconfigurableslit cryogenic configuration slit software in mask use usedKeck at in Observatory) Keck MOSFIRE that at allows Keck. masks Right: to be The reconfigured in 3 minutes. (From: W.M. to MOSFIRE. 3.1.1.3 Wide Field Optical Spectrograph - WFOS several years ago (see Figure Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources scopic capability has a high scientific priorityat for this TMT. time, Several design including concepts a areutilizing being deployable pre-made explored fiber slit masks. fed A system, baseline imageillustrate design the slicers that capabilities was and that previously a developed can is more be described traditional expected here for system to WFOS regardless of the final design. PoS(MULTIF2017)082 14 Image of the MOBIE design for WFOS. Light enters from the right. The large scale of the Of particular relevance to studies in many areas of high energy cosmic sources isRapid the ability response for depends on two factors, 1; the physical ability of the observatory to slew, As previously mentioned, TMT has the most stringent requirements for rapid response of all of Maunakea on Hawaii Island was selected in 2009 as the site for TMT after a long site testing an observatory to respond rapidly and carry out Target of Opportunity (ToO) observingchange programs. and configure instruments and for manyimages cases the to rapid the delivery of instruments, adaptive 2; opticsToO corrected having programs the and appropriate respond operational rapidly procedures (ideally automatically) in to place alerts. to pre-define the ELTs with a 10 minuteobservations maximum on response another from target ending at onecapability a observation different for to position studies beginning with science of asupport different many queue instrument. types scheduled This observations of and is that transient aToO ability critical program objects. allows by the interrupting possibility The the of queue. observatory rapid execution is of being a designed to 3.1.4 TMT Construction Timeline and selection process. TMT beganseveral exploring candidate construction sites) in and Hawaii establishing in local 2003 employment, workforce (whilst development investigating and education Figure 9: instrument is seen. A significantenough. technical challenge (Credit: for TMT this International design Observatory) is the fabrication of optics that are large 3.1.3 Queue scheduling and Target of Opportunity Observations Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources PoS(MULTIF2017)082 15 Flowchart showing the instrument development process for post-first light instruments for TMT The Thirty Meter Telescope will provide exciting capabilities that will enable many different In order to move forward, in 2016 a call for proposals to host TMT was distributedOn-site construction and has after been rescheduled to restart in early 2018 at either Maunakea or ORM. Construction is scheduled to last about 10 years and will transfer to operations when the tele- ]. This process will be repeated every 2 to 3 years to ensure a regular arrival of new instruments to the 6 studies of high energy astrophysicalscales. sources and Strong high synergies energy will processes existfacilities over with that small other operate to astronomical cosmic at facilities, size be other they wavelengths, survey gravitational telescopes wave or observatories, neutrino or cosmic 4. Conclusions observatory. The first cycle is beginningthe now TMT as construction the timescale. development timescale of about 10 years is the same as programs from about 2009. The projectrevocation entered of the the construction building phase permit in at 2014 the but end protests of and the 2015 have createdconsidering delays. the possible alternate siteschos a (ORM) final on selection the of Island Observatorio of del La Palma Roque as de the los alternate Mucha- siteFor for both TMT sites, was the made. fullare legal processes being of followed seeking at theconstruction necessary this restart permissions date. time to and begin construction the final decision of whichscope and site some will of be theThis first made is light closer planned instruments for to are the delivered late the and 2020s. science commissioning has begun. Figure 10: [ Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources PoS(MULTIF2017)082 16 The instruments will all be located on the Nasmyth platforms at the sides of Will the instrument platform move with the mirror or will it remain stationary? cluster galaxy lens", Science, 347, p1123 the 10 kpc core of Abell 3827", MNRAS, 449, p3393 emission-line galaxy with precessing radio jets", MNRAS, 465, p4772 http://goo.gl/MwzMHV [1] Skidmore, W., 2015, "Thirty Meter Telescope Detailed[2] Science Case:Kelly, P., 2015", et RAA, al., 15, 2015, p1945 "Multiple images of a highly magnified supernova[3] formed byMassey, an R., early-type et al., 2015, "The behaviour of dark matter associated with[4] four brightRubinur, cluster K., galaxies Das, in M., Kharb, P., Honey, M., 2016, "A candidate dual[5] AGN in aSimard, double-peaked L., et al., 2010, "The[6] TMT InstrumentationSimard, Program", L., SPIE, et 7735, al., 23-1 2015, "Planning Future TMT Instruments", TMT2G Workshop Possibilities for comprehensive studies involving the TMT of the ’zoo’ of high energy sources ray detectors. The rapidversatile and response powerful capabilities tool for and the range exploration of of the instrument high capabilities energy universe. willReferences create a DISCUSSION Paul Mason: Warren Skidmore: the telescope, these platforms arethe part of vertical the axis telescope of structurefor the and the will center instruments. move of in When the azimuth the(located around telescope. in telescope the moves middle This in of the provides altitude primaryis to a mirror) selected. follow will constant track an vertical and object, send gravity the the vector beam tertiary to mirror which ever instrument