The Detailed Science Case of the Maunakea Spectroscopic Explorer

The Detailed Science Case of the Maunakea Spectroscopic Explorer

The Detailed Science Case of the Maunakea Spectroscopic Explorer The MSE Science Team April 9, 2019 2 i Contents Preface to Version 2 of the Detailed Science Case, 2019 vii Preface to Version 1 of the Detailed Science Case, 2016 xi 1 Executive Summary 1 2 The scientific landscape of the Maunakea Spectroscopic Explorer 5 2.1 The composition and dynamics of the faint Universe . 6 2.2 MSE and the international network of astronomical facilities . 13 2.2.1 Optical imaging of the Universe . 14 2.2.2 Wide field optical and infrared science from space . 16 2.2.3 Multi-messenger and time-domain astronomy . 17 2.2.4 The era of Gaia . 18 2.2.5 Synergies at long wavelengths . 21 2.2.6 30m-class telescopes and MSE . 25 2.3 From science cases to facility requirements . 26 2.4 From science cases to a science platform . 28 2.5 The science capabilities of MSE . 30 2.5.1 Key capability 1: survey speed and sensitivity . 31 2.5.2 Key capability 2: spectral performance and multiplexing . 32 2.5.3 Key capability 3: dedicated and specialized operations . 33 2.5.4 Development of the multi-object IFU mode . 34 2.6 Competition and synergies with future MOS . 35 2.7 A scientific priority for the coming decade of discovery . 36 3 Exoplanets and stellar astrophysics 39 3.1 Introduction . 40 3.2 Information content of MSE stellar spectra . 40 ii 3.3 Exoplanets and substellar mass objects . 42 3.3.1 Radial velocity surveys . 42 3.3.2 Characterization of transiting exoplanets . 45 3.3.3 Characterisation of exoplanet and brown dwarf atmospheres . 45 3.3.4 Exoplanet host stars and proto-planetary disks . 48 3.3.5 Planetary systems around white dwarfs . 50 3.4 Stellar physics with star clusters . 52 3.4.1 Pre-main sequence stars . 53 3.4.2 Open clusters . 54 3.4.3 Globular clusters . 57 3.4.4 White dwarfs . 58 3.5 Asteroseismology, rotation, and stellar activity . 59 3.5.1 Solar-like oscillations . 59 3.5.2 Stellar activity and rotation . 61 3.5.3 Opacity-driven pulsators . 62 3.6 Stars in multiple systems . 63 3.6.1 The binary census in the Milky Way and Local Group galaxies . 64 3.6.2 Eclipsing binaries . 66 3.6.3 Wide binaries as probes of post-main sequence mass loss . 66 3.6.4 Compact white dwarf binaries . 67 3.6.5 Massive stars as progenitors of compact object mergers . 68 3.7 Asymptotic giant branch evolution . 69 3.8 Very metal-poor stars . 71 4 Chemical nucleosynthesis 73 4.1 Motivation: From BBN to B2FH . 74 4.2 Metal-poor stars and the first chemical enrichment events in the Universe . 75 4.3 The cosmological lithium problem . 76 4.4 The promise and potential of chemical tagging to probe the origin of the elements . 78 4.5 Sites of i-process and the origin of the CEMP-r/s stars . 80 4.6 Studying AGBs and their progeny . 81 4.7 Survey of r-process elements . 83 4.8 Nucleosynthesis and chemical evolution in dwarf galaxies . 85 5 The Milky Way and resolved stellar populations 89 5.1 Context: Galactic archaeology in the era of Gaia . 90 iii 5.2 The chemodynamical evolution of the Milky Way . 95 5.2.1 The Galactic disk . 95 5.2.2 The Galactic bulge . 96 5.2.3 The stellar halo . 97 5.3 In-situ chemical tagging of the outer Galaxy . 98 5.4 First stars and the progenitors of the Milky Way . 101 5.5 The Local Group as a time machine for galaxy evolution . 105 5.5.1 The chemodynamical deconstruction of the nearest L* galaxy . 108 5.5.2 Dwarf galaxies . 112 5.5.3 Globular clusters . 115 5.6 The interstellar medium . 117 5.6.1 3D mapping the Galactic ISM . 117 5.6.2 Three-dimensional ISM mapping: MSE perspectives . 119 5.6.3 Targetted studies of the ISM . 122 6 Astrophysical tests of dark matter 127 6.1 Motivation . 128 6.2 How can astrophysics probe the particle nature of dark matter? . 130 6.2.1 Dark matter physics . 130 6.2.2 Observables . 133 6.2.3 The impact of baryons . 134 6.3 Stars and stellar streams in the Milky Way . 135 6.3.1 Mapping the Milky Way’s gravitational potential with stars, dwarf galaxies, and stellar streams . 136 6.3.2 Dark matter halo distortions from the LMC in the MW halo . 138 6.3.3 Identifying the dark sub-halo population with stellar streams . 142 6.3.4 Local dark matter distribution and kinematics for direct detection . 145 6.3.5 Dark matter distribution in the Galactic Center for indirect detection 146 6.4 Dwarf galaxies in the Milky Way and beyond with resolved stars . 147 6.4.1 Luminosity function of Milky Way satellites in the era of LSST . 149 6.4.2 Precise determination of the J-factor of nearby ultra-faint dwarf galaxies151 6.4.3 Controlling systematics with spatial and temporal completeness at high resolution . 152 6.5 Galaxies in the low redshift Universe . 155 6.5.1 The faint end of the galaxy luminosity function . 155 6.5.2 Satellite populations in Milky Way analogs . 157 6.5.3 Local galaxies as gravitational lenses . 159 iv 6.5.4 Ultra diffuse galaxies . 160 6.6 Galaxies beyond the low redshift Universe . 162 6.6.1 Quasar lensing: flux ratio anomalies due to low mass dark matter halos163 6.6.2 Galaxy-galaxy lensing: image perturbations by low mass dark matter halos . 166 6.6.3 Wobbling of the brightest cluster galaxies . 168 7 Galaxy formation and evolution 171 7.1 Extragalactic surveys with MSE . 172 7.1.1 Local Universe wide-field surveys . 175 7.1.2 High redshift surveys . 176 7.1.3 Ancillary surveys . 179 7.2 Large scale structure and galaxy halos . 181 7.2.1 IGM tomographic mapping . 181 7.2.2 Halo occupation modelling in the Local Universe . 182 7.2.3 Galaxy groups/clusters at z ∼ 2 − 3 ................... 185 7.2.4 Satellite planes in the nearby universe . 185 7.3 Massive galaxies . 188 7.3.1 Mapping giant galaxy assembly at z ∼ 0 with compact stellar systems 188 7.3.2 A census of massive galaxies at cosmic noon . 190 7.3.3 Star formation & stellar assembly histories . 191 7.3.4 Environment & mergers . 192 7.4 M?galaxies (Milky Way analogues) . 194 7.4.1 Star formation/stellar assembly histories . 194 7.4.2 Co-evolution of AGN and galaxies . 196 7.5 Dwarf galaxies . 198 8 Active Galactic Nuclei and Supermassive Black Holes 203 8.1 Context . 204 8.2 The central engine: supermassive black holes and accretion . 204 8.2.1 How are SMBHs seeded in galaxies? . 204 8.2.2 Measuring SMBH masses: Reverberation Mapping the Inner Regions of Quasars . 206 8.2.3 How do SMBHs grow? AGN triggering mechanisms and different fuelling/accretion modes . 207 8.2.4 Measuring accretion in real-time: extreme variability, tidal disruption events and changing-look AGN . 209 v 8.2.5 Binary SMBHs . 210 8.2.6 Outflows from SMBHs as traced through BALs and intrinsic NALs . 211 8.3 AGN host galaxies . 212 8.3.1 AGN host galaxies and type-2 AGN . 212 8.3.2 From the epoch of re-ionization – high-z AGN and their hosts . 215 8.3.3 AGN feedback . 216 8.4 Beyond the host galaxy – cosmological aspects and applications of AGN and SMBHs . 218 8.4.1 AGN clustering and demography . 218 8.4.2 Gravitational lensing applications . 219 8.5 QSO (intervening) absorption line applications . 222 9 Cosmology 227 9.1 Motivation . 228 9.1.1 Background cosmology . 228 9.1.2 The role of galaxy redshift surveys . 229 9.2 A high redshift cosmology survey with MSE . 231 9.2.1 Survey baseline . ..

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