PoS(FRAPWS2018)085 https://pos.sissa.it/ ∗† [email protected] Speaker. Sincere thanks to Franco Giovannelli for the invitation! After its launch, the James Webb Space Telescopespace (JWST) mission will become in one the of history. the most Thisarea important mid-infrared mirror ever telescope sent will to benefit the fromexplore, space. the along many largest A other collecting set interesting of observations, many theobserve various dawn the instruments of very will the first allow Universe at stars the high scientists andthree redshifts, to scientific galaxies to as tasks are well highlighted: asIII to the stars; look JWST and at deep follow-up selected observations field; exoplanets. of acounterpart. short search In gamma-ray for this bursts with lensed article the very aim distant to Pop detect a kilonova † ∗ 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). Frontier Research in Astrophysics - III (FRAPWS2018) 28 May - 2 June 2018 Mondello (Palermo), Italy Dublin Institute of Advanced Studies, SchoolIreland of Cosmic Physics, 31 FitzwilliamE-mail: Place, Dublin, Martin Topinka JWST - The Even Bigger Time Machine PoS(FRAPWS2018)085 m to µ Martin Topinka 1 ], often presented as the next generation Hubble Space 2 , 1 14 m), JWST will become the largest space telescope mission ever × A concept of JWST with the primary mirror, the secondary mirror, the sun shield and the space- . With the segmented primary gold-coated mirror 6.6 m in diameter, made of 18 segments JWST will be an infra-red telescope, optimised for the wavelength range from 0.6 The design of the telescope covers the primary and the secondary mirror, the spacecraft bus The mission life time, mostly determined by the fuel for manoeuvring, is expected to be around The James Webb Space Telescope [ 1 Figure 1: craft bus and star-trackers. Credit: NASA. 2. Instruments On-Board and the sun shield amongure the instruments and detectors.in The Beryllium, overall enhanced build with is an depictedsize active in of optic the a system, Fig- tennis together court with (26 the m bus and the sun shield of a 10 years, with the minimum engineered time of 5 years. Telescope, is being constructed as a collaborationand the between Canadian NASA, Space European Agency Space (CSA). Agency Thethe (ESA) project Northrop is Grumman lead by company Goddard as Space thestitute flight is prime Centre, responsible having constructor, for while the the telescope Space operation.side Telescope The of Science involvement the in In- co-operation the a project gives guaranteed the minimum European of 15% of the observing time. launched. JWST 1. Introduction PoS(FRAPWS2018)085 ]: NIRCam, 3 Martin Topinka . The process will take two 2 and changes over time as the observatory ◦ 12 months. The orientation of the telescope and to 135 2 ∼ ◦ A depiction of the JWST deployment on its way to L2. Credit: NASA/GSFC. Figure 2: m to be able to observe distant galaxies, "cool" objects and to peer into very dusty environ- JWST has four (or five, depends on the definition) main instruments on board [ Due its size the deployment resembles an origami unfolding from the compact state in the To diminish the IR radiation background noise, the telescope will be deployed at the L2 point µ NIRSpec, NIRISS and MIRI (and the fly guidance star tracker). Their field of views are not co- cargo head of a launchingand rocket. erect the JWST secondary will mirror on "unpack" the the way solar to array, L2, the as seen sun in shield, the the Figure mirror the geometry of the sun shield withof respect regard to the extends Sun from limits a the solar viewingorbits directions. elongation the The of sun. JWST 85 field of the Earth-Sun system orbit,pull 1.5 of million the kilometres Earth-Sun from system the the Earth. period will Thanks be to the gravitational JWST 28 ments. The size of the mirror,background the radiation detector will sensitivity enable and a the lowto telescope level the to of mid- gather the infrared a telescope range infra-red very self of faintthe signal the near from spectrum. infrared. the An A near-infrared angular 6.5-meterand resolution diameter provides is a primary similar very mirror to good diffraction the pointing limited HST stability. is one at but around in 2 microns weeks from the launch. PoS(FRAPWS2018)085 , . 7 3 , 6 , 5 , 4 Martin Topinka . The telescope is 4 40 K by the sun shield, except MIRI cooled ≈ C). 3 ◦ ]. 12 . The photometric and spectroscopic performance of [ 233 4 5 − ]. MIRI has a set of coronagraphs: the traditional Lyot and the Four Quadrant Phase The JWST instrument FOVs are pointing towards the same direction, however, they are not co- 11 , 10 C), while the dark side stays at 40 K ( Most of the instrument are passively cooled to JWST capabilities includes imaging, spectroscopy, multi-object spectroscopy, slit-less spec- The Near Infrared Camera (NIRCam) is JWST’s primary imager that will cover the infrared , ◦ 9 , to 7 K. The sunwith silicon shield on has the been sun side designed(85 and to aluminium have on the 5 other layers surfaces. made Thus, of the sun heat-resistant side Kapton reaches 358 coated K sensitive enough to detect the heatMoon. radiated The from sensitivity a plot bee is flying in on the the Figure distance from the Earth to the troscopy, integrated field unit spectroscopy,ferometry. single object There coronography is and asimultaneously aperture possibility with mask to a inter- properly define chosen parallel dither observationsthe pattern, size the with only of combining limitation the two is on-board the buffer instruments link when band submitting width the and data to the Earth. Masks ones. The Fine Guidance Sensorhigh-quality (FGS) allows images. JWST to The point precisely, Near soFGS that Infrared has it Imager can a obtain and wavelength range Slit-lessboard of Spectrograph JWST 0.8 (NIRISS) are to summarised part 5.0 in of microns. the the Figure The capabilities of the main instruments on- wavelength range 0.6 to 5Spectrograph microns. (NIRSpec) NIRCam will is equipped operate withNIRSpec also is coronagraphs. over designed The the to Near observe wavelength InfraRed upin range to space of 100 that objects has 0.6 this simultaneously. to remarkable Itboth multi-object 5 will a capability. be microns. camera The the Mid-Infrared and first The Instrument spectrograph a8 (MIRI) spectrograph has covering the wavelength range of 5 to 28 microns [ Figure 3: centric. Parallel observations require a specific dither pattern. Credit: NASA/STScI. the instruments, beating HST and Spitzer is shown in the panels of the Figure JWST centric, their FOV orientations with respect to the telescope pointing axes are shown in the Figure PoS(FRAPWS2018)085 – Martin Topinka – What are the first galaxies – When and how does the re- – How do clouds of gas and dust collapse to form 4 ]: 14 , 13 A summary of the capabilities of the JWST main scientific instruments. Credit: NASA. Being more than one order of magnitude sensitive in some bandsThe than first any half other year observatory, is of the operation will be dedicated to commissioning and calibration of The end of the dark ages, the first lightExoplanets and and re-ionisation planetary systems (including our solar system) and the origins of life Birth of stars and protoplanetary systems Assembly of galaxies, the formation and evolution of galaxies Four essential astrophysical fields have been selected as the main objectives of the mission, Figure 4: a lot of unpredicted discoveries are expected. the instruments. The data acquired duringEarly this Release period Science will be (ERS) released programme. for public immediately in the How are the building blocks of planetsthat assembled? give rise What to are planetary the systems? constituents Doafter of planets forming circumstellar in in disks a the planetary outer system reaches form of inof place, the stars or system? travel where Can inwards it we is find planets possible orbiting for in water, the or habitable perhaps zones life, to exist? Was there ever life on Mars? like? How are galaxiesgalaxies? formed? What happens How when do small the and large central galaxies black collide holes or join in together? ionisation galaxies occur? influence What their sources host caused it? stars? How do planetary systems form? described in great details in [ 3. Scientific Goals JWST PoS(FRAPWS2018)085 ≤ ∼ AB Martin Topinka 6 galaxies. The plan is to 6 galaxies. The imager will − 30 lensing clusters to 4 ≥ − z ∼ for cluster transverse velocities of 17, gravitationally lensed by a galaxy 5 − 10 7 − ∼ 4 z 3) emitters. By the UDF, JWST can constrain . 10 11 5 ' − 6. Thanks to the instrument sensitivity it can detect 10. The UDF will lead to determination of the Star 9 . 10. This will allow the scientists to look for the most ≥ > 8 z z − ∼ 5 z ∼ z 4) and [OIII] ( . 8 − 6 . 6 ∼ . Depending on BH masses, accretion-disk radii and feeding efficiencies, stellar-mass Comparison of sensitivity of the JWST instruments with existing missions. Credit: NASA. 1 z ( − s α b) Another brave proposal is the aim to observe a signal from a single Population III stars and From the vast ocean of proposals fora) observations, The here the JWST attention Ultra-Deep is Field drawn (UDF) to is three of planned them: to go beyond the limits reached by the HST Figure 5: 1000 km BH accretion-disk caustic transitsPopulation could outnumber III those caustic from transits Population directly III may stars. require To to observe monitor 3 their BH accretion disks at the very large redshifts use combined NIRCam and MIRIsurveyed instruments by in Spitzer parallel and with HST) ditheringto field over benefit which the from yields GOODS-S the 255 (also full sq. wavelength range arcmin of at the 25h, telescope. 40h, 60h exposure times cluster. Typical caustic magnifications can be in projects, spanning the redshifts 4. Highlighted Contribution Formation History for the galaxies with strong H the Galaxy Stellar Mass Functiondetermine and Cosmic the Stellar morphology Density of for the old stellar populations in the z distant intermediate mass objects in the JWST PoS(FRAPWS2018)085 Martin Topinka ]. MIRISim allows users 20 , 19 . 6 ]. The emission is believed to be a summarises the delays and the cost 25 1 ]. There-in you can find links to the Exposure 16 6 ]. The coincidence positive gravitational wave detection is not 26 ], has been observed later on [ 24 ]. ]. So far, discovered in a similar fashion, the record bearer is a HST ]. Moreover, a near and/or far infra-red counterpart of a sGRB, called a 22 21 23 ]. For advanced end-to-end simulations of the observations with the MIRI 5 [ . 18 1 , = 17 z 10 micron, as simulated in [ The least favourite and the most discussed aspect of the JWST mission is a further heavy delay There are several software tools being developed to make the life of a JWST scientist easier. c) The most promising theory for a short gamma-ray burst (sGRB) proposed so far is that − 5 of its launch that has been announced recently. The Table to see a simulated datacubethrough as the the result MIRI of detector. observingparameters A the such sources user as on the can customised the customise input skyexample the sky predefined of scene, virtual by the dither observation workflow patterns, a using defined number user MIRISim of by is integrations, a etc. shown in variety An the of Figure 6. Delay of the Launch Date instrument, the MIRISim software package has been developed [ Time Calculator (ETC) and Astronomersthe Proposal observations Tool [ (APT) that are ready to use for planning The extensive user documentation is accessible [ product of the r-process in the neutron-richthe environment around collimated the gamma-ray apocalyptic NS emission merger.to Unlike lasting be for spherical an and eye-blink,great may the details last to kilonova for further emission days. prove istheir the evolution. JWST expected sGRB-kilonova scenario is A and call capable to for toa inspect a obtain detected the Target a of spectral afterglow Opportunity spectrum features and/or (ToO) and ofhas for a such been precisely neutron source submitted localised star sGRB in in burst merger cases∼ with with the a gamma-ray burst detected occursnecessary and in in well this the ToO. localised reach afterglow of the MIRI instrument at 5. JWST Software increase, starting from the initial costmain and launch reason date for estimate the in 1997 latestresults up delay, of to vibration communicated today’s tests situation. by that The the leadand NASA to improving headquarters, a its partial unfolding is redesign mechanism. the of The unsatisfactory extra the NASA time sun strategy in shield, is testing clear the rather that choice than it of losingpoint is the the makes better entire materials any to spacecraft service since spend or parking some repair the5 satellite mission with around impossible. the the To L2 JWST this folded date, in the the launch cargo of top the of rocket the Ariane rocket has been scheduled for March 2021. kilonova, proposed in theory [ observation of the most distantat star the lensed redshift by of a cluster, Icarus MACS J1149+2223 Lensed Star 1, JWST 29 mag over a decade [ the progenitor is a binarydirect observation neutron of the star gravitational (NS) waves GW170817 merger. detectedmatching by the the A LIGO-VIRGO template breakthrough experiment of in aby this neutron the theory star FERMI merger was satellite and a [ coinciding recent with a sGRB counterpart detected PoS(FRAPWS2018)085 Martin Topinka 10 8.8 ≥ ≥ 7 Year Launch Budget Plan (Billion USD) 199719981999 2007 2007 to2000 2007 200820022003 20092005 20102006 2011 0.5 1 2008 2013 1 2010 2014 2015 to2011 2014 2016 1.8 2013 2.5 2017 2018 2.5 2018 2018 3 2019 6.5 4.5 2020 5.1 8.7 8.8 8.8 2018 2021 The estimated launch dates and the expected costs of JWST. Credit: Wiki. Table 1: An example of MIRISim in action, starting from a scene description in a text file (left) to a All instruments are now fully integrated with the telescope and they areIf performing things to go the well, the JWST telescope will dominate the IR astronomy domain in the next Figure 6: 7. Conclusion specs. A detailed review ofafter the every launch. single The component reasonable has launch been date, planned currently estimated to today, diminish is anydecade March 2021. flaw thanks at to or its uniquequestions on outstanding early star capabilities. and galaxy It formation inand will the for Universe, bring uncover the sure, answers composition of to it exoplanets many will fundamental also bring many new unexpected discoveries. Fingers crossed that all the simulated output image on theprivate communication. detector (right). Credit: Pamela Klaassen on behalf of the MIRISim team, JWST PoS(FRAPWS2018)085 Martin Topinka 8 https://www.jwst.nasa.gov https://jwst.stsci.edu/instrumentation http://docs.jwst.nasa.gov https://jwst.etc.stsci.edu http://www.stsci.edu/hst/proposing/apt https://miricle.org [1] Clampin, M. 2008, Advances in Space[2] Research, Vol. 41, 1983 [3] [4] Rieke, G. H., Wright, G. S.,[5] Böker, T., etWright, al. G. 2015, S., PASP, Vol. Wright, 127, D., 584 Goodson,[6] G. B.,Bouchet, et P., al. García-Marín, 2015, M., PASP, Vol. Lagage, 127, P.-O., 595 et[7] al. 2015,Kendrew, PASP, S., Vol. 127, Scheithauer, 612 S., Bouchet, P., et[8] al. 2015,Boccaletti, PASP, Vol. 127, A., 623 Lagage, P.-O., Baudoz, P., et[9] al. 2015,Wells, PASP, Vol. M., 127, Pel, 633 J.-W., Glasse, A., et al. 2015, PASP, Vol. 127, 646 JWST construction issues would be solved andachieve many JWST great would new be discoveries! launched and deployed successfully and References [10] Rieke, G. H., Ressler, M. 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