Submitted Abstracts
TMT-AGE: AO-assisted wide field multi object spectrograph concept
By: Masayuki Akiyama
Abstract: We have been conducting a feasibility study on a wide field of regard (FoR) AO-assisted NIR multi-object spectrograph as a second generation instrument (TMT-AGE: TMT-Analyzer for Galaxies in the Early universe). In this study, we put emphasis on the AO-assisted FoR as wide as 10 arcmin diameter. The wide FoR is crucial to conduct statistical observations on very high-redshift galaxies, which have low surface number density. In this talk, we will introduce possible overall system designs of the instrument.
Stellar physics and galactic archaeology with high resolutions spectroscopy
By: Wako Aoki
Abstract: High resolution spectroscopy is essential in stellar physics and galactic archaeology. A large progress is expected in these fields with TMT. I'll review recent discoveries and discuss expected function for high resolution spectrometers of TMT.
International Collaboration in Astronomy for Asia - Strategy of Subaru Telescope
By: Nobuo Arimoto
Abstract: Strategy of Subaru for international collaboration with Asian communities will be presented. Several topics include current status of Subaru’s operation, a decommission plan of instruments, new generation instruments (HSC, PFS, ULTIMATE ), Subaru strategic programs, strategy of Subaru for 2020’s synergy with TMT and Space. Ambitious plan for the international operation of Subaru with Asian countries will also be mentioned briefly.
Science In the Era of the 30m With the Brightest Lensed Galaxies In the Observable Universe
By: Matthew Bayliss
Abstract: Wide-field surveys of large fractions of the sky reveal on the order of a hundred strongly lensed high redshift galaxies that are highly magnified and optically bright (AB magnitude ~<21). After the era of LSST is underway, we will have imaged essentially the entire extra-galactic sky, and will therefore have the data available to identify all of the brightest lensed galaxies in the observable universe. These lensed galaxies will forever constitute a unique and finite number of opportunities for probing the astrophysics of galaxy evolution and star formation at high redshift. As we move forward toward future generations of observational facilities it is important to remain cognizant of the opportunities that are within reach when we combine state-of-the-art man made facilities with the most exceptional natural telescopes that are serendipitously available. In this talk I will summarize some recent results from observations of the brightest known lensed galaxies on 8m class facilities, and discuss the prospects and promise for studying these systems with the next generation of 30m class facilities.
Co-Authors: M. Gladders, J. Rigby, K. Sharon, H. Dahle, T. Johnson, M. Florian, K. Whitaker
Does the Stellar IMF Evolve with Redshift?: Insights from GRBs and Field Galaxies
By: Ranga Chary
Abstract: The ubiquity of strong nebular emission lines in z > 3 galaxies, the enhancement of long-duration gamma-ray burst rates relative to the comoving star-formation rate density and evidence for a discrepancy between stellar mass density and integral of star-formation rate densities have challenged our understanding of star-formation in distant galaxies. An increase in the ionization parameter through an evolution of the stellar IMF is a panacea to these issues and can be physically motivated, but is challenging to measure. I will discuss how a two-pronged TMT key program involving 1) spectroscopy of z > 3 gamma-ray burst afterglows to measure their redshifts and intervening metallicities of the ISM; and 2) spectroscopy of 3 < z < 5 star-forming galaxies in the near-infrared which allows nebular line strengths to be measured, will be a powerful approach to testing this hypothesis. The synergy between TMT and JWST for high-redshift emission-line diagnostics will also be discussed.
Characterization of brown dwarfs and planetary mass objects in young star clusters
By: Wen-Ping Chen
Abstract: I outline the plan to study brown dwarfs and planet-mass objects in young star clusters. The majority of known brown dwarfs are in the field, i.e., already evolved. Brown dwarfs and planet-mass objects are relatively bright at birth and, with no sustaining thermonuclear energy source, fade rapidly. Yet substellar objects even out to the nearest star-forming regions (beyond 130 pc) are mostly too faint to identify and characterize with existing instruments. Current approach relies on identification of candidates by imaging photometry typically with mid-sized telescopes, either with broad-band filters to trace cool atmospheres, or with molecular band filters to trace possible a specific absorption features (e.g., methane or water). After contamination of active galaxies or young variables is winnowed, follow-up spectroscopic confirmation is required for each candidate using telescopes with large apertures. But even 8 to 10 meter class telescopes often fall short to render sufficient signals to diagnose physical and chemical parameters precisely enough to constrain cool atmospheric models. I will describe the ongoing efforts and how TMT may contribute to the characterization from the lowest-mass star members, to brown dwarf and planet-mass members of young star clusters in order to understand the the interplay of origins of stellar
and substellar masses.
Co-Authors: Poshih Chiang Manash Samal
The European Extremely Large Telescope
By: Michele Cirasuolo
Abstract: I will present an overview of the E-ELT Programme including the key science drivers and an update on the current status of telescope and instrumentation.
Co-Authors: E-ELT Programme
Some Considerations for High Resolution IR Spectroscopy at the TMT
By: Tim Davidge
Abstract: In this brief talk I will discuss the IR spectral region, with emphasis on the $1 - 5\mu$m interval, and suggest ways for improving observing efficiency.
TMT Capabilities and Instrumentation for Galaxy Cluster Cosmology
By: Ian Dell'Antonio
Abstract: I will describe the key contributions TMT could make to cluster cosmology, and discuss the first light and second epoch instrumentation that would enable these contributions
Co-Authors: Gillian Wilson Michael Pierce Marusa Bradac Tommaso Treu Marie Lemoine-Busserole
An international partnership for operating TMT
By: Christophe Dumas
Abstract: In this talk, we will discuss strategies for shaping TMT operations using the international nature of its partnership.
After an initial period dedicated to AIV and observatory commissioning, steady state operations will require a science and technical staff of about 120 persons. Daytime technical presence on the summit will address the support of all engineering and maintenance activities, while a minimal nighttime crew will be present at the telescope to secure safe night-operations of the equipment.
As part of TMT international partnership, we can foresee a network of remote observing sites to be geographically distributed throughout TMT’s member states and institutes. These centers could be designed to support the specific needs of each partner's scientific community and reflect their poles of expertise. By supporting observation preparation, execution, and possibly data-reduction/analysis, these centers will foster collaboration and grow knowledge across the partnership.
The execution of the approved science programs will be implemented in the schedule in a manner to optimize scientific outputs. Programs with stringent observing constraints, or time-critical components (e.g. 'Target of Opportunity’ programs), will be fully supported, and all science data, and their associated calibration frames, will be archived and made available to the whole community of TMT users.
Co-Authors: TMT-DEOPS team-members
TMT High-Contrast Exoplanet Science
By: Michael Fitzgerald
Abstract: The detection and characterization of other planetary systems promises to be a rich and exciting field over the coming decade, in particular with the expected and imminent scientific return of GAIA, TESS, and JWST. Looking to the TMT era, we expect tantalizing progress in addressing how planetary systems form and evolve, understanding our solar system’s uniqueness within the diversity of such systems, and giving the first glimpses into the nearby systems most suitable for future exploration. TMT will be one of several facilities poised to make an impact in these exciting areas. I will discuss those areas in which high-contrast exoplanet imaging and spectroscopy on this large ground-based telescope will be unique in the latter half of the next decade, and why a dedicated high-contrast facility instrument is critical to achieve this impact. I will also discuss how precursor technology development instrumentation and activities can make unique scientific contributions along the way to such a facility instrument.
Co-Authors: Ben Mazin
High Resolution Optical Spectroscopy in the ELT Era
By: Cynthia Suzanne Froning
Abstract: The development of seeing-limited high resolution spectrographs for the visible waveband brings special challenges in the ELT aperture regime. Here, I will summarize the design drivers for such instruments, highlight the technical challenges, and present a novel conceptual design for TMT-HROS.
Tracking Jupiter’s Quasi-Quadrennial Oscillation and Mid-Latitude Zonal Waves with High Spectral Resolution Mid-Infrared Observations
By: Thomas Greathouse
Abstract: We report on early results of a long term observational study to track the temporal and 3-dimensional evolution of the Quasi-Quadrennial Oscillation (QQO) and the propagation and evolution of mid-latitude zonal waves in Jupiter’s stratosphere. These wave-driven phenomena affect variations in Jupiter’s vertical and horizontal temperature field, which can be inferred by measuring methane emission in the thermal infrared at 1245 cm-1. Using TEXES, the Texas Echelon cross-dispersed Echelle Spectrograph, mounted on the NASA Infrared Telescope Facility (IRTF) we observed high-spectral resolution (R=75,000) scan maps of Jupiter’s mid-latitudes from January 2012 thru the present. We will present the zonally averaged inferred thermal structure over ±30° latitude and between 10 and 0.01 mbar, showing the QQO’s downward progression along with inferred 3-dimensional thermal maps (latitude, longitude, pressure) displaying a multitude of vertically isolated waves and eddies. These results reveal a vast array of wave activity on Jupiter and will serve to: 1) significantly improve the determination of the period and vertical descent velocity of Jupiter’s QQO; 2) measure the zonal wavenumbers, vertical wavelengths, zonal group velocities and lifetimes of transient mid-latitude waves; and 3) record the thermal state of Jupiter’s stratosphere in detail prior to, during, and after Juno’s prime.
Co-Authors: T.K. Greathouse, G.S. Orton, R. Morales-Juberias, L.N. Fletcher, C.N. DeWitt, R. Consentino
A Fast Path to Imaging and Characterizing Habitable Exoplanets around the Nearest Stars with TMT
By: Olivier Guyon
Abstract:
Thanks to their large apertures, ELTs will be able to resolve habitable zones of nearby M-type stars in the near-IR. The planet-to-star reflected light contrast around these targets (approximately 1e-7 to 1e-8) is achievable with a combination of coronagraphy, extreme-AO correction and PSF calibration, allowing for the first time spectroscopic characterization of nearby habitable exoplanets.
We describe a path to seize this opportunity on TMT near first light, by deploying an instrument optimized for high contrast imaging of a small sample of nearby stars. We propose to evolve the Subaru Coronagraphic Extreme-AO (SCExAO) instrument toward a TMT instrument. The key technologies (small inner working angle coronagraphy, fast pupil plane and focal plane wavefront sensor, spectroscopic calibration) will be validated on the 8-m Subaru Telescope over the next few years, yielding a system-level performance validation prior to deployment on TMT. This approach provides a rapid, cost-effective path towards spectroscopic characterization of exoplanets. The proposed program will also feed into the design and operation (including control and data processing algorithms) of a more capable second generation instrument with a broader set of science goals, and will characterize the telescope performance in the context of high contrast imaging.
Co-Authors: Motohide Tamura Nemanja Jovanovic Julien Lozi Tomoyuki Kudo Ben Mazin Michael Fitzgerald Taro Matsuo Jared Males Dimitri Mawet Ji Wang Takayuki Kotani Hajime Kawahara
Supermassive Black Holes with TMT and its Future-generation Instruments
By: Lei Hao
Abstract: In this talk, I will overview a few aspects on studies of supermassive black holes and active galactic nuclei at various redshifts. I will particularly mention a few science cases that may not be covered by the 1st-generation instruments.
Exploring the nature of Lyman alpha galaxies at z~2-6 using large VLT spectroscopic surveys: A prelude to TMT science
By: Nimish Hathi
Abstract: A comprehensive analysis of star-forming galaxies (SFGs), including a crucial sub-population of Lyman alpha emitters (LAEs), at high redshifts (z>2) using multi-wavelength photometry and deep spectroscopy is vital for understanding the physical processes that govern the star formation activity and galaxy assembly through cosmic time. Until now, such studies were limited to small number of galaxies because of the lack of large area, deep observations at high redshifts. With extensive multi-wavelength photometry from the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS), and deep ground-based spectroscopy from the VIMOS Ultra-Deep Survey (VUDS) and a VIMOS deep survey of the CANDELS fields (VANDELS), we can now investigate physical properties of a large sample of SFGs/LAEs at z~2-6. I will present results from recent studies based on spectroscopic and photometric data of SFGs/LAEs at high redshift. TMT's high resolution spectroscopy coupled with deep multi-band imaging from JWST will enable us to do a more thorough investigation at z<6, while allowing us to probe the faintest, most distant galaxies, to better understand the nature of SFGs/LAEs as well as their role in the reionization process.
Developing an International Training Program for TMT
By: Lisa Marie Hunter
Abstract: The Institute for Scientists and Engineer Educators (ISEE) is working with the Thirty Meter Telescope International Observatory (TIO) community to design a program to benefit all of the TIO partner sites in Japan, China, India, Canada, and the U.S. The program will provide a unique opportunity for training tomorrow’s scientific and technological leaders, while also strengthening collaborations across TIO partner sites. The goals in the design phase of this project include learning about TIO partners’ interests and priorities, developing the basic design for the program, and then reviewing the basic design with the TIO community to shape the details. Currently, the basic design includes a 2-week annual retreat for selected graduate students from every partner country. At this retreat, international teams of students will be formed and collaborate on proposing an approach to a current TIO problem or area of interest. Participants will also receive a variety of technical, leadership, and cross-cultural training, which will continue after the retreat ends as the teams continue to collaborate virtually. Finally, the proposed program will culminate in a select few of the retreat participants traveling abroad and working at one of the partner sites on his or her proposed project under senior leadership. The goal of this talk is to stimulate thoughts, comments, ideas, or suggestions that will shape the final design of a program that will be beneficial to the full TMT partnership.
Co-Authors: Austin Barnes
The Instrumentation Program for the Giant Magellan Telescope
By: George H Jacoby
Abstract: Instrument development for the 24 m Giant Magellan Telescope (GMT) will be described: current activities, progress, status, and schedule. One instrument team completed its preliminary design and is beginning its final design (G-CLEF, an optical 350-950 nm high-resolution and precision radial velocity echelle spectrograph). A second instrument team (GMACS, an optical 350-950 nm low-to-medium resolution 6-10 arcmin field multi-object spectrograph) is starting a new conceptual design. A third instrument team is midway through its preliminary design (GMTIFS, a near-IR YJHK diffraction-limited imager/integral-field-spectrograph), focused on risk reduction. A fourth instrument team (GMTNIRS, a JHKLM high-resolution AO-fed echelle spectrograph) is fabricating the 5 silicon immersion gratings it needs prior to preliminary design. And, another instrument team is completing a small-scale science demonstrator instrument (MANIFEST, a facility robotic multi-fiber-feed with a 20 arcmin field of view). In addition, a medium-field (6 arcmin, 0.07 arcsec/pix) optical imager has been added that will excel at narrow-band imaging. In the spirit of advancing synergies with other groups, I will discuss the challenges of running an ELT instrument program, lessons learned, and opportunities for cross-ELT collaboration.
The Future of Infrared Surface Brightness Fluctuation Distance Measurements
By: Joseph Jensen
Abstract: Surface brightness fluctuations (SBF) are a means for measuring precise distances to early-type galaxies. We have calibrated the SBF method for the Wide Field Camera 3 IR channel (WFC3/IR) on the HST, making it possible to measure accurate distances out to ~100 Mpc in a single orbit. To extend the technique to greater distances, we have recently developed the IR SBF techniques for MCAO using the GeMS system on Gemini. From the ground, near-IR observations using adaptive optics on TMT will achieve much higher spatial resolution, enhancing the SBF signal. The HST and Gemini measurements show how JWST and TMT may be used to extend the IR SBF distance technique to 500 Mpc.
Co-Authors: John Blakeslee
Probing accretion processes through variability
By: Vishal Pramod Kasliwal
Abstract: The accretion of mass onto a compact object is thought to be mechanism responsible for powering luminous objects such as BH-XRBS, quasars and other AGN. A characteristic feature of accretion onto a compact object is pan-spectral optical variability in the continuum of the SED. The observed variability is highly-aperiodic with a broadband power-law powerspectrum. The underlying physical origin of the variability is not understood though models range from inward-propagating accretion rate fluctuations caused by changes in the local viscosity to MHD turbulence generated by the MRI responsible for enabling accretion. Local hot spots may form in the accretion disk giving rise to the observed fluctuations. Continuum variability arises in the accretion disk itself, therefore it can be a powerful probe of accretion physics.
AGN variability has been modeled as a damped random walk (DRW). More recently, the statistical model has been generalized to higher-order DRWs known as Continuous-time Auto-Regressive Moving Average (C-ARMA) processes. We present a physical interpretation of these statistical models in which processes such as thermal dissipation and turbulent mixing smear out the hot spots formed by MHD processes. The smearing is characterized using a Green's function approach. We have developed a fast C++ & Python software package to model light curves as C-ARMA processes. We apply our software and method to the Kepler light curve of the Sy 1 AGN Zw 299-15 and find that hot spots in the accretion disk quickly brighten in luminosity reaching peak amplitude after ~ 5 d after which they gradually decay with an e-folding timescale of ~ 70 d. We discuss on-going efforts to apply our methods to light curves generated by combing SDSS Stripe 82 data with data from NASA's K2 mission.
Co-Authors: Michael S. Vogeley Gordon T. Richards Adam Lidz
NIR High-resolution spectrographs for the TMT
By: Naoto Kobayashi
Abstract: In the last decade, there have been significant improvements in sensitivity and efficiency of NIR (0.9-5.5 micron) high-resolution spectrographs (HRSs) thanks to the technical advances, such as large-format infrared arrays and novel gratings. With high-quality spectra as for optical-HRSs, NIR-HRS is becoming one of the ubuquitous tools in astronomy to study all kinds of astronomical objects. In particular, NIR-HRS for the TMT should provide unique opportunities to challenge fundamental physics and chemistry. In this talk, I will briefly outline several instrumental solutions for NIR-HRSs for the TMT: one is NIRES-B, which covers 0.9-1.8um (YJH-bands), and the other is NIRES-R or MICHI-B, which covers 2-5um (K-,L-,M-bands).
Co-Authors: Yuji Ikeda (Photocoding) Hideyo Kawakita (Laboratory of IR High-resolution spectroscopy, Koyama Astronomical Observatory)
Morphologies and building blocks of galaxies at high redshift
By: Mariko Kubo
Abstract: Hierarchical build-up scenario of galaxies is predicted in the several high resolution cosmological numerical simulations in the Lambda CDM cosmology. Although we hardly test this scenario to date.
From our own deep NIR imaging and spectroscopic observations of the protocluster at z=3.09 in the SSA22 field, which is one of the most significant structure in the Universe, we found several dense groups of galaxies at z_spec=3.09. The most extreme case of these groups very resembles to the early-phase or multiple merger phase of brightest cluster galaxies predicted in the cosmological numerical simulations.
We studied the morphologies of the members of this proto-BCG like galaxy group by using the deep and high resolution K-band imaging data obtained by using IRCS/AO188 on Subaru Telescope.
We found that the most massive member (M*~2x10^11 M_sun), maybe the main progenitor, is an compact elliptical with effective radius re ~1 kpc. On the other hand, other members in the group have the sizes on average larger than those of field SFGs at the same redshift. Our results imply strong size evolution of BCG from z=3 and the environment dependance of its building blocks for the first time.
Based on these new results, I would like to discuss the science cases of morphologies and behaviors of faint end of high redshift galaxies in the framework of hierarchical galaxy formation scenario, studied with the deep and high resolution imaging with TMT.
Co-Authors: Toru Yamada (ISAS/JAXA), Takashi Ichikawa (Tohoku Univ), Masaru Kajisawa (Ehime Univ), Yuichi Matsuda (NAOJ, Soken-dai), Ichi Tanaka (NAOJ) and Hideki Umehata (IoA)
Extremely low-mass star-burst galaxies at $z\sim2.2$
By: Haruka Kusakabe
Abstract: Low-mass galaxies at high redshift play a key role in galaxy formation and evolution as progenitors of more massive galaxies seen at later epochs. We study on star formation properties and their diversity of Lyα Emitters (LAEs) at $z\sim2.2$, a commonly seen low-mass galaxy population. We divide 604 LAEs in the SXDS field into sub-samples based on the distribution of four UV physical parameters: MUV, $\beta$ , L(Ly$\alpha$), and EW(Ly$\alpha$). The halo mass and stellar population parameters for each sub-sample are calculated from clustering analysis and SED fitting, respectively. While two thirds of the entire sample are on the star formation main sequence with stellar masses of $\sim10^9 M_{\odot}$, the remaining one third, which are the lowest-mass objects in our sample, are forming stars burstly with stellar masses of $\sim10^7 M_{\odot}$ and sSFRs $\sim10^{-7}-10^{-6}yr^{-1}$. Their SFRs exceeds the baryon accretion rates of their hosting halos. These low-stellar mass LAEs may be in initial forming phases at cosmic noon. We will also discuss the future work on their detailed star-formation physics and structures revealed by AO and IFU of TMT.
Co-Authors: K. shimasaku, K. Nakajima, R. Goto, M. Ouchi, T. Hashimoto, A. Konno, Y. Harikane, Y. Ono
Unraveling the Nature of Dust Production from Wolf-Rayet Binaries
By: Ryan M Lau
Abstract: The dust contribution from Wolf Rayet stars with close O/B-star companions to the dust budget of galaxies in the local and early Universe has been largely neglected. Carbon-rich WR (WC) stars, identified by broad C emission lines, stars are unique amongst WR stars since many are observed to produce up to 10^-6 M_Sun yr^-1 in dust. A majority of these dusty WC stars are in binary systems with an O/B-star companion: strong winds from the WC star collide with weaker winds from the companion and create dense regions in the wake of the companion's orbit that are shielded from the harsh radiation fi eld and allow for dust to condense. The tell-tale signature of this dust formation process is a remarkable "pinwheel". Although the dust formation is clearly linked to the presence of the WC-star, the details of how dust forms and survives in such hostile environments is still uncertain. With the unprecedented angular resolution of the Thirty Meter Telescope, we will be able to study the morphology and energetics of the newly formed dust in WC binaries and unravel the nature of their dust production.
Co-Authors: M. J. Hankins, M. R. Morris, J. Sanchez-Bermudez, J. U. Pott, J. D. Adams, T. L .Herter, M. E. Ressler
Mapping the z=2-4 Intergalactic Medium with Lyman-alpha Forest Tomography
By: Khee-Gan Lee
Abstract: I will discuss the technique of Lyman-alpha forest tomography, in which faint z~2-3 LBGs and quasars at small sightline separations are observed in order to measure their foreground Lyman-alpha forest absorption. This is then reconstructed to obtain the full 3D absorption field of the IGM, which will reveal the cosmic web at these high redshifts. Pilot observations are now underway with Keck, but TMT will revolutionize this technique by targeting faint (>25th mag) galaxies at sufficient number densities to fully resolve <1Mpc scales.
Co-Authors: Martin White, Joe Hennawi, Xavier Prochaska, David Schlegel
Constraining dark matter identity with strong gravitational lensing
By: Ran Li
Abstract: The cold dark matter (CDM) cosmological model unambigously predicts that a large number of haloes should survive as subhaloes when they are accreted into a larger halo. The CDM model would be ruled out if such substructures were shown not to exist. By contrast, if the dark matter consists of warm particles (WDM), then below a threshold mass that depends on the particle mass far fewer substructures would be present. Finding subhaloes below a certain mass would then rule out warm particle masses below some value. Strong gravitational lensing provides a clean method to measure the subhalo mass function through distortions in the structure of Einstein rings and giant arcs. Using mock lensing observations constructed from high-resolution N-body simulations, we show that measurements of ~100 strong lens systems with a detection limit of Mlow = 10^7h^{−1}M⊙ would clearly distinguish CDM from WDM in the case where this consists of 7 keV sterile neutrinos such as those that might be responsible for the 3.5 keV X-ray emission line recently detected in galaxies and clusters.
Morphology and Composition of the Dusty Torus in Active Galactic Nuclei
By: Enrique Lopez Rodriguez
Abstract: The high-spatial resolution observations provided by TMT in combination with the wide wavelength coverage provided by IRIS (0.8-2.4 um) and MICHI (3-13 um) will be able to resolve and to image, for the first time in the infrared, the dusty torus of active galactic nuclei (AGN). This talk will present a science case focused on the investigation of the morphology and composition of the dusty torus in AGN. Simulated images of the dusty torus using clumpy torus models in the 1-13 um wavelength range will be shown as well as the expected observing times and TMT requirements to achieve the goals of this project.
Co-Authors: K. Ichikawa, N. Levenson, R. Nikutta, C. Packham
Prospects for the Extragalactic Distance Scale with TMT
By: Lucas Macri
Abstract: I will briefly review the present status of the Extragalactic Distance Scale and summarize the progress expected in the next few years. I will discuss the prospects for future work on this topic once TMT becomes operational, focusing on synergies with LSST and JWST.
A TMT Cosmic Web Imager (TCWI)
By: Christopher Martin
Abstract: We discuss the scientific case and conceptual design of a high-performance integral field TMT spectrograph for the 3000-10500Å band. The scientific potential for such an instrument is enormous, ranging from young star evolution to mapping cold inflow proto-galactic disks to imaging the cosmic web. I present a concept for a moderate-cost TCWI using the existing KCWI design.
Co-Authors: Matt Matuszewski, Patrick Morrissey, Anna Moore
Planet Detection and Characterization at High Contrast
By: Ben Mazin
Abstract: The direct imaging of exoplanets from the ground will reveal the nature of the exoplanets in the solar neighborhood in a way that is not possible with any other technique. The large aperture of TMT will allow measurements of planets very close to their primary star, potentially in the habitable zone of nearby low-mass stars. To pursue this vital research we are forming a cross-partnership team of experts to develop the scientific and technological requirements of a high-contrast TMT exoplanet instrument with the primary goals of both detecting rocky planets in reflected light, and larger planets at high spectral resolution. In this talk we will summarize the science drivers of this instrument, and then delve into the requirements of this instrument’s modules. We will also discuss a roadmap of the technological progress required to enable TMT to be the first observatory to achieve these goals.
Co-Authors: Michael Fitzgerald
HeNOS, the NFIRAOS AO simulator at NRC-Herzberg
By: Etsuko Mieda
Abstract: The development of adaptive optics (AO) facilities is crucial for fully utilizing the high resolution capabilities of Extremely Large Telescopes. In this presentation, I will describe the components and functions of a TMT multi-conjugate (MC) AO simulation bench at NRC-Herzberg, called the HeNOS (Herzberg NFIRAOS Optical Simulator) bench. Its purpose is to validate the NFIRAOS calibration procedures and control algorithms by comparing simulated performance with real data acquired in a controlled environment. The HeNOS bench is currently at the final alignment stage, which includes a truth wavefront sensor based on a double pyramid. Once it is completely assembled and fully running, it will be used to validate PSF reconstruction in real-time on an MCAO system, which is a critical functionality to enable quantitative astronomy with AO, but has proved to be a very challenging problem.
Co-Authors: M. Rosensteiner, J. Veran, O. Lardiere, G. Herriot
Infrared Spectroastrometric Imaging of the Water Snowline and C/O Ratio Distributions in Protoplanetary Disks
By: Shota Notsu
Abstract: The location of the water snowline in protoplanetary disks is crucial to understand planet formation process since it is thought to divide the regions between rocky and gas giant planet formation. It will also give us fundamental information on how water was delivered to Earth. However, spatial resolution of the existing telescopes is insufficient to directly image the water snowline. Here we propose to detect the water snowline by spectroastrometric imaging using high dispersion spectroscopic observations. Mid-infrared water line emission at 18$¥mu$m and 25$¥mu$m are the best to trace the water snowline, according to our simulations based on sophisticated physical and chemical disk modeling. The spectroastrometric method to measure the line emitting regions has been established using the 4.7$¥mu$m CO lines.
High dispersion and high sensitivity observations by TMT/MICHI enable us to detect the water snowline in large numbers of protoplanetary disks. Moreover, emission lines other than water, such as HCN, will be observable simultaneously. They are useful to trace the distributions of carbon-to-oxygen ratio in disks. Statistical observations to compare the location and atmospheric composition of exoplanets with the location of snowlines and the distributions of carbon-to-oxygen ratio in disks will constrain the formation process of short period planets.
Co-Authors: H. Nomura, M. Honda
Solar-System Observations from the Thirty-Meter Telescope
By: Glenn Scott ORTON
Abstract: Potential observations of solar-system objects enabled by the TMT will be reviewed. For objects that are unresolved spatially, the TMT provides the advantage of sensitivity, enabling detection of faint objects by imaging and spectroscopy and the increase of spectral resolution. This can be applied to asteroids, Kuiper-Belt Objects (KBOs), distant comets and members of satellite systems. For objects that are resolvable, a substantial increase of spatial resolution is possible by minimizing diffraction limits, particular in the near- and mid-infrared. This includes large satellites, such as Titan with its thick and time-variable atmosphere, Io with active volcanism, the atmospheres of Uranus and Neptune, and portions (or full mosaics) of Jupiter and Saturn – all with spatial resolution previously available only by nearby spacecraft.
Subaru Near-Infrared Spectroscopy for Young Brown Dwarfs and Planetary Mass Objects
By: Yumiko Oasa
Abstract: We present the results of NIR multi-object spectroscopy with Subaru/MOIRCS for very low-luminosity young stellar objects.
Their spectroscopic temperatures, together with their bolometric luminosities, indicate that they could be substellar-mass YSOs such as brown dwarfs and isolated planetary-mass objects.The mass functions steadily increase toward completeness limit which is below the deuterium-burning limit.
We expect that TMT will detect not only a significant population of substellar-mass objects but also disks around planetary mass objects.
Co-Authors: Yusuke Takahara, Yoichi Itoh
MICHI (未知), A Thermal IR Instrument Concept for the TMT
By: Chris Packham
Abstract: A thermal-IR (optimized for ~3-14μm) imager/spectrograph is being investigated for possible construction in the early operation of the TMT. Combined with the mid-IR adaptive optics (AO) system, MIRAO, the instrument will afford ~15 times higher sensitivity at ~4 times higher spatial resolution (0.07”) at 10μm compared to 8m-class telescopes, and at much higher Strehl ratios (~4 times better). Additionally, through exploiting the large collection area of the TMT, a high-dispersion spectroscopy mode will be unrivaled by other ground- and space-based facilities. These combined capabilities offer the possibility for breakthrough science, as well as ‘workhorse’ observing modes of imaging and low/moderate spectral resolution. We are making a detailed study of if MIRAO-fed observing in the early daytime hours would be feasible. In this presentation we summarize the primary science drivers that are guiding the instrument development.
Co-Authors: C. Packham (Texas, NAOJ), M. Honda (Kanagawa), Y. K. Okamoto (Ibaraki), M. Chun (Hawaii), H. Kataza (ISAS/JAXA), T. Onaka (Tokyo), M. Richter (Davis), I Sakon (Tokyo), And the 未知 Science & Instrument Team
GAS: the Galaxy Assembly Spectrograph
By: Michael Jay Pierce
Abstract: One of the key science programs being discussed for TMT is the characterization of the assembly history of disk galaxies at z > 1. NIFIRAOS+IRIS will provide integral-field spectroscopy of these systems and allow their disk kinematics, star formation rates and abundance gradients to be measured. However, acquiring the necessary data for a sample of 50 galaxies in each of 3-5 redshift bins will be very expensive. An alternative approach is to develop a spectroscopic capability with deployable integral-field units that can operate over the entire AO-corrected field of view of TMT. With this goal we propose the Galaxy Assembly Spectrograph (GAS). GAS would use about 100 cryogenic robotic positioners with fiber arrays similar to those used in MaNGA. Each 200-fiber IFU would feed an individual but identical spectrograph. This approach would allow each spectrograph to be individually configured according to its target's redshift, and the desired resolution and wavelength range requirements. The TMT+NIFIRAOS focal plane will rank with
some of the most valuable real estate on the planet and the high multiplexing capability of GAS would maximize the use of TMT resources in the study of z > 1 galaxies.
Stars, Gas, and the Milky Way: Science for 2nd Gen Instruments
By: Catherine A Pilachowski
Abstract: The new Thirty Meter Telescope Detailed Science Case: 2015 (Skidmore et al. 2015) outlines many challenging research frontiers that require extremely large aperture telescopes to reach. First generation TMT instruments will resolve many of these science questions, but for stars and the interstellar medium in the Milky Way, key observations will await second generation instruments. In this talk I will review a few of the big stellar and Galactic astrophysics questions to be addressed with TMT and its suite of second generation instruments, with a focus on the critical capabilities that will be needed.
Star and planet formation studies with TMT
By: Manoj Puravankara
Abstract: In this talk, I will briefly summarize the research interests of the Indian astronomy community in the field of star and planet formation and describe the efforts that are currently underway in planning for science with TMT. I will then discuss one key science case in detail that attempts to characterize early protostellar evolution with TMT, by measuring mass flow rates associated with infall, accretion and outflows in protostars as a function of system age.
The Resolved Stellar, Chemical, and Gaseous Contents of High-Redshift Galaxies
By: Naveen Reddy
Abstract: I will discuss some of the recent progress in understanding the resolved stellar, chemical, and gaseous contents of high-redshift galaxies, focusing on those studies that benefited from the capabilities of ground-based optical telescopes like Keck. I will then outline a few open questions that will benefit from AO-assisted instrumentation planned for TMT.
The Study and Search for Intermediate and massive Black Holes in the Local Group/Volume
By: Robert Michael Rich
Abstract: The search for intermediate mass black holes in Globular clusters remains a frustrating endeavor with only a single case (M31-G1) still considered strong, although there is no radio detection of G1*. I will discuss opportunities to improve existing data on, and survey for additional, IMBH in nuclei and globular clusters. I will also consider studies of the nuclei of M31, M32, M33, and NGC 205. Initial assays of these systems will be supplemented by a highS/N WFOS survey, with IRIS being used to obtain images and IFU spectra at the highest resolution of TMT. In order to detect well IMBH of the mass of G1*, 2e5Msun, R~8000 spectroscopy is needed. Multiple IFU and mid-IR instruments are appropriate 2nd generation candidates, as well as extreme AO that might achieve correction shortward of 9000A.
TMT Observations of GRBs & SNe as Early Universe Probes
By: Pete Roming
Abstract: Gamma-ray bursts (GRBs) and supernovae (SNe) are among the best tools for probing the early Universe, but are still as yet essentially unexploited. Massive stars that end their lives as GRBs have been proposed as tools for measuring the star formation rate out to high redshift. These earliest generations of stars could be surveyed, assuming that Pop III stars end their lives as GRBs. Because of their intrinsically featureless synchrotron spectra, GRBs have also been proposed as a means of investigating the reionization history along different sight lines as well as probing local host environments in the early Universe. Pair-instability supernovae (PISN) and Type IIn SNe can also be used as a tool for measuring the massive star formation rate and their contribution to the chemical enrichment in the early Universe. I will focus on the utility of GRBs and SNe as cosmological probes and TMT’s critical role in their use.
Theoretical prediction for the detectability of z > 7 nebular lines
By: Ikko Shimizu
Abstract: We have performed very large and high resolution cosmological hydrodynamic simulations in order to investigate detectability of various nebular lines in the rest-frame ultraviolet (UV) to optical wavelength range from galaxies at z > 7. We find that metal lines such as CIV 1549A and the CIII] 1909A can be good targets for the spectroscopic observation with Thirty Meter Telescope (TMT).
We also predict detectability of the nebular lines for z > 10 galaxies that will be found with Wide-Field Infrared Survey Telescope (WFIRST) and First Light And Reionization Explorer (FLARE) (11 < z < 15). We conclude that the CIV 1549A and the CIII] 1909A lines even from z ~ 15 galaxies can be strong targets for TMT.
Co-Authors: Akio, K. Inoue (Osaka Sangyo University); Naoki, Yoshida (University of Tokyo); Takashi Okamoto (Hokkaido University).
TMT Instrumentation: First Light and Beyond
By: Luc Simard
Abstract: The Thirty-Meter Telescope international observatory will enable transformational observations over the full cosmic timeline all the way from the first luminous objects in the Universe to the planets and moons of our own solar system. To realize its full scientific potential, TMT will be equipped with a powerful suite of adaptive optics systems and science instruments. I will give an update on our three first-light instruments (WFOS, IRMS and IRIS) as well as the NFIRAOS Science Calibration Unit (NSCU) and our facility instrument cryogenic cooling system. I will also discuss plans for future generation instruments for TMT.
Stellar abundances in stars and ISM: probes of stellar physics and Galaxy formation
By: Thirupathi Sivarani
Abstract: We present stellar abundances (mainly the light-elements Li, Be, CNO and n-capture elements) as probes of stellar evolution process. A good understanding of mechanisms of their production and astrophysical sites is crucial to use them as tools to understand galaxy formation, evolution and cosmology. We highlight the capabilities of TMT in reaching fainter magnitudes, adaptive optics and blue sensitivity to address these problems.
Co-Authors: A. Susmitha Rani, A. Bandyopadhyay, W. Aoki, T.C. Beers, P. Bonifacio, N. Christlieb, A. Koch, J. Ge
Thermal Imaging of Gas Giants and Rocky Planets with TMT
By: Andy Skemer
Abstract: The TMT will make fast progress in detecting and characterizing extrasolar planets in the thermal infrared. I will review what thermal imaging has taught us about our own Solar System and other planetary systems, and discuss some of the exciting possibilities that will be enabled by the TMT, including the detection of self-luminous gas-giant planets, and rocky planets. The technologies required for these science cases is mature and capable of ground-breaking, yet low-risk science early in the TMT's lifetime.
The Science Flowdown Process - From the Science Case to Science Requirements
By: Warren Skidmore
Abstract: A large range of observing programs have been identified from the many varied science programs mentioned in the TMT 2015 Detailed Science Case. The 2015 DSC contains ideas for science programs that were developed by the TMT International Science Development Teams. The ISDT members have been asked to provide technical information for the observing program or programs that are in their area of expertise. This technical input will be used to update the science requirements for the observatory.
The overal science flowdown process is described and a status given for the gathering of technical input.
Co-Authors: With the assistance of the TMT ISDTs.
TMT Workforce, Education, Public Outreach and Communications - A Global Plan
By: Gordon K. Squires
Abstract: TMT science and technology is international in scope, meaning that TMT strives to be an observatory-class facility for astronomers in all of the partner constituencies. In this presentation, we will provide an update on the goals, opportunities, and needs for developing a partnership-wide Workforce, Education, Public Outreach and Communications (WEPOC) plan to support the key elements of the TMT observatory and partnership. Central to this plan is the commitment to be relevant and responsive to all of the partners, fully leverage all phases of the project, and project forward through the 50 year lifetime of the observatory. I will also provide an update on WEPOC activities specifically designed for TMT in Hawaii.
Co-Authors: Janesse Brewer, Sandra Dawson, Steve Pompea, Nanci Dumas, Azusa Minamizaku & the TMT WEPOC Advisory Group
Radial metallicity gradients form MOS observations of emission-line probes: Constraining galactic chemical evolution.
By: Letizia Stanghellini
Abstract: We present a summary of recent results on galactic metallicity gradients from emission-line probes in star-forming galaxies. H II regions and planetary nebulae (PNe) abundances give a handle on the evolution of radial metallicity gradients with time. Apart form the Galaxy, most of the data have been collected with MOS technology. Direct abundances of H II and PNe are within reach only for a handful of galaxies with current capabilities and by using 8m-class telescopes; current results, while relevant, are statistically limited. We discuss how this field will greatly profit from future 30m-class telescope MOS.
Cosmology with Time Domain TMT observations
By: Nao Suzuki
Abstract: In the era of TMT, cosmological parameters would be listed as a table on your textbook, and students would take them for granted, while "the great ocean of truth lay all undiscovered before" us. TMT would change the way we study the cosmology. I will highlight a few exciting topics in the context of time domain science.
New distance indicators, Fast Radio Burst (FRB) and Gravitational Wave as a standard siren are suggested but they may need redshift measurement from TMT. Reverberation Mapping of AGNs enters new era if we can resolve the dust torus with TMT. Cepheid variable measurements can be extended to cosmological distances, and we may be able to find inhomogeneous expansion of the local universe.
In 2020s, millions of supernova would be discovered by LSST but only TMT can probe the nature of dark energy in the decelerating universe with Type Ia supernova (SNIa). For the first time, we should be able to see the companion star of nearby exploded SNIa which would help us understand the diversity of SNIa. The holy grail of supernova observation is to find a 'First Star' and its explosion. TMT would be the first to discover them.
Ultimately, TMT should be able to see the expansion of the universe directly from the IGM aborption line shifts with 10-year-interval. The definition of time domain would be changed by TMT.
The Impact of TMT on Close Binary Research
By: Paula Szkody
Abstract: While large telescope science tends to concentrate on distant objects and early epochs of the universe, there are also important applications for nearby, low brightness sources in the Milky Way and nearby galaxies. An example of this is the research on numerous close binary systems that will interact through mass transfer at some point in their evolution. I will summarize the main science issues in cataclysmic variables that will benefit from TMT, including results from observations of the component stars, the effects of magnetic fields and mass transfer on these stars and how population determination can provide insights into evolution paths. The optimum TMT instrumentation to realize advances in this field will be discussed.
Feasibility of Spectro-Polarimetric Detection of Atmospheric Components of Exoplanets
By: Jun Takahashi
Abstract: We present the result of our feasibility evaluation of spectro-polarimetric detection of atmospheric components of extrasolar planets. Model calculations by Stam et al. (2004) and Stam (2008) predicted that a polarization degree spectrum of reflected light from a planet has enhanced features at absorption wavelengths of the atmospheric molecules such as methane, water, and oxygen. Besides, polarization degree is considered to be insensitive to telluric absorptions because polarimetry is a relative measurement, Thus, spectro-polarimetry of exoplanets may be used for detection of those molecules, even on the ground.
Motivated by those benefits of spectro-polarimetry, we evaluate feasibility of spectro-polarimetric detection of water vapor in an exoplanet atmosphere. It is assumed that we will use a high-contrast spectro-polarimeter on a 30-40m class ground-based telescope. We consider several types of errors including (a) the error from different instrumental efficiencies between uncommon optical paths for ordinary and extra-ordinary light beams, (b) the error caused by the speckle noises, and (c) errors from the photon noises. Based on the calculated values of the errors, we estimate the number of planets which will allow effective spectro-polarimetric search of water vapor. The result indicates that spectro-polarmetric search of water vapor is feasible for some of the known planets.
References
Stam, D. M. 2008, A&A, 482, 989
Stam, D. M., Hovenier, J. W., & Waters, L. B. F. M. 2004, A&A, 428, 663
Co-Authors: Taro Matsuo (Osaka University), Yoichi Itoh (University of Hyogo)
TMT and Gravitational Wave Astronomy
By: Masaomi Tanaka
Abstract: In 2015, Advanced LIGO has detected the first ever direct gravitational wave (GW) signals from a black hole merger. This discovery marked the dawn of GW astronomy. One of the most important next steps for GW astronomy is conclusive identification of the electromagnetic counterpart. In particular, optical and near-infrared emission is expected from neutron star mergers, and many wide-field transient surveys are hunting for this emission. To firmly identify the GW sources, spectroscopic observations are required. I will talk on the importance of TMT for gravitational wave astronomy, and review what we will learn from "multi-messenger" observations.
TMT Key Science Program Discussion
By: Tommaso Treu
Abstract: I will summarize the outcomes of the first simulated call for Key Science Program Proposals, and lead a discussion on the topic.
Time-Domain Sciences in the Era of TMT
By: Xiaofeng Wang
Abstract: Time-domain exploration of the universe has become one of the frontier pursuit in modern astronomy and astrophysics as the exisiting sky surveys have incessantly revealed new types of celestial transients. This field is expected to continue its growth over the coming decades, with the start of ever larger sky surveys such as the Large Synoptic Survey Telescope (LSST). In this talk, I will discuss a few interesting time-domain science cases that may benefit from the powerful capabilities of optical/near-infrared spectroscopy of the TMT. This includes the studies of progenitors of various SNe and GRBs, SN and GRB cosmology, accretion physics of CVs, and tidal disruption events etc.
Co-Authors: All members of the TMT Time-domain ISDT.
Na I D lines in Type Ia Supernovae by TMT
By: Kaicheng Zhang
Abstract: Type Ia supernovae (SNe Ia) have been used as cosmological standard candles to research the expansion history of the universe for many years, but their progenitor system remains unclear. There are two possible scenarios to explode a SN Ia: 1). two CO white dwarfs merge, says double-degenerate (DD) scenario; or 2). one CO white dwarf accretes material from its non-degenerate companion, says single-degenerate (SD) scenario. In SD scenario, the progenitor system will blow away matter to form a circumsteller material (CSM) shell, while in DD scenario it is not expected to happen. Na I D absorption lines are good indicators for the CSM around SNe Ia, as already been studied in many previous works. The TMT first generation instrument WFOS (R $\sim$ 5000) has the capability to resolve Na I D lines at 5890\AA and 5896\AA. There is little research on the evolution of Na I D absorption in very early phase spectrum. But to check ionization models, it is critical to get very early phase data. We can use TMT+WFOS to study the existence and evolution of Na I D lines in the spectra of SNe Ia in order to help constrain their progenitor models.
Co-Authors: Wenxiong Li, Xiaofeng Wang
