Surface Telerobotics 1

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2 DARE Project Team Principal Investigator: Jack Burns, University of Colorado Boulder Project Management & Mission Operations: NASA Ames Research Center: B. Hine & J. Bauman Observatory Project Management: Ball Aerospace & Technologies Corp.: W. Purcell & D. Newell Science Co-Investigators: Robert MacDowall, NASA GSFC, Project Scientist Richard Bradley, NRAO, Deputy Project Scientist Judd Bowman, Arizona State University Abhirup Datta, University of Colorado Boulder Anastasia Fialkov, CfA Steven Furlanetto, UCLA Dayton Jones, Space Science Institute, Boulder Justin Kasper, University of Michigan Joseph Lazio, JPL/Caltech Abraham Loeb, Harvard University Raul Monsalve, ASU & U. Colorado Jordan Mirocha, UCLA Collaborators: Michael Bicay, NASA Ames William Farrell, NASA GSFC Jonathan Pritchard, Imperial College Eric Switzer, NASA GSFC Edward Wollack, NASA GSFC Graduate Students: Bang Nhan, University of Colorado Keith Tauscher, University of Colorado 2

3 The First Half-Billion Years The First Stars John Wise, Georgia Tech z=1100 z~20-30 z~6 Dare Science Questions When did the First Stars ignite? What were these First Stars? When did the first accreting Black Holes turn on? What was the characteristic mass? When did Reionization begin? Any signs of exotic physics (e.g. Dark Matter decay) from global signal? 5

4 The 21-cm Hyperfine Line of Neutral Hydrogen 40 MHz z 35 6

5 The 21-cm Line in Cosmology > (P=kT b Δν) Courtesy of J. Pritchard 7

6 The 21-cm Global Signal Reveals the Birth & Characteristics of the First Stars & Galaxies B: ignition of first stars When did the First Stars ignite? What were these First Stars? What surprises emerged from the Dark Ages? C: heating by first black holes When did the first accreting black holes turn on? What was the characteristic mass? D: the onset of reionization When did Reionization begin? --- uncertainties in 1st star models --- uncertainties in 1st black hole models Adapted from Pritchard & Loeb, 2010, Phys. Rev. D, 82, and Mirocha, Harker, & Burns, 2015, ApJ, 813, 11. 8

7 Range of Model Parameters for 1 st Stars & Galaxies Courtesy of Jordan Mirocha ARES ( Accelerated Reionization Era Simulations) code 9

8 Astrophysics Decadal Survey & Astrophysics Roadmap identify Cosmic Dawn as a top Science Objective A great mystery now confronts us: When and how did the first galaxies form out of cold clumps of hydrogen gas and start to shine when was our cosmic dawn? New Worlds, New Horizons (NRC 2010) How Does our Universe Work? Small Mission: Mapping the Universe s hydrogen clouds using 21-cm radio wavelengths via a lunar orbiter observing from the farside of the Moon NASA Astrophysics Division Roadmap (2013) What were the first objects to light up the Universe and when did they do it? We can uniquely address this mystery with DARE in orbit above the lunar farside. 11

9 Observational Approaches for Detection of Global 21-cm Monopole Single Antenna Radiometers EDGES (Bowman & Rogers) SARAS (Patra et al.) LEDA (Greenhill, Bernardi et al.) SCI-HI (Lopez-Cruz, Peterson, Voytek et al.) BIGHORNS (Sokolowski et al.) DARE (Burns et al.) Challenges include systematics arising from stability issues, accurate calibration, polarization leakage, foregrounds. Small, Compact Interferometric Arrays Vedantham et al. Mahesh et al. Presley, Parsons & Liu Subrahmanyan, Singh et al. Challenges include cross-talk among antenna elements, modecoupling of foreground continuum sources into spectral confusion, sensitivity. 12

10 Ground-Based Heritage Ground-based telescopes generally operate at >100 MHz & probe only the end of the Epoch of Reionization (EoR) Single Antenna, Total Power: EoR Global Signal Interferometric Arrays: Measure Power Spectrum of EoR LOFAR - Europe MWA Western Australia Experiment to Detect the Global EoR Step = EDGES (Bowman & Rogers) Total power receiver; 3 position Dickeswitch to calibrate spectrum. New antenna topologies. New wide-band receiver. Set first limits on Reionization step function. PAPER South Africa Evolving into HERA 320 element array =>In contrast, DARE will measure Global Cosmic Dawn monopole down to 40 MHz, a measurement requiring a lunar-orbiting telescope. 13

11 Single Antenna Diagram has been modified from a LOFAR presentation by S. Zaroubi ( 14

12 Foregrounds: Major Challenge Earth s Ionosphere (e.g., Vedantham et al. 2014; Datta et al. 2016; Rogers et al. 2015; Sokolowski et al. 2015) o o o Refraction, absorption, & emission Spatial & temporal variations related to forcing action by solar UV & X-rays => 1/f or flicker noise acts as another systematic or bias. Effects scale as ν -2 so they get much worse quickly below ~100 MHz. Radio Frequency Interference (RFI) o o o RFI particularly problematic for FM band ( MHz). Reflection off the Moon, space debris, aircraft, & ionized meteor trails are an issue everywhere on Earth (e.g., Tingay et al. 2013; Vedantham et al. 2013). Even in LEO (10 8 K) or lunar nearside (10 6 K), RFI brightness T B is high. Galactic/Extragalactic o o Mainly synchrotron with expected smooth spectrum (~3 rd order log polynomial,, although it is corrupted by antenna beam; e.g., Bernardi et al. 2015). EDGES finds spectral structure at levels <12 mk in foreground at MHz. Other Foregrounds - lunar thermal emission & reflections; Jupiter; Recombination lines. 18

13 Lunar Farside: No RFI or Ionosphere! (z=46) RAE (z=13) 19

14 Extraterrestrial Foregrounds 1) Milky Way synchrotron emission + sea of extragalactic sources. DARE beam Spectra of Foregrounds 2) Solar system objects: Sun, Jupiter, Moon. =>Must employ advanced statistical techniques to simultaneously fit signal, foregrounds, & instrument parameters 20

15 Beam Measurements Circularly polarized, PSK modulated carriers (6) are sent from ground to DARE. DARE receives signals as the spacecraft orbits above near side of the Moon to sweep beam. Carrier levels are measured by DARE every 20 seconds to produce sampled beam cut. A weak signal is also measured on its return trip to the Earth (Moon reflection) to estimate real-time path loss through the ionosphere. 23

16 Precision Calibration: Tone Injection Weak 21-cm signal against bright foregrounds requires high dynamic range measurement. Need precise measurements of gain drifts in the radiometer. Classical Dicke switching is not accurate enough. Narrow frequency tone (few khz) injected. Voltage ν tone is measured with high fidelity demonstrated in lab to 50 db. 24

17 Polarimeter: Removal of Foreground Cosmic Twilight Polarimeter: Ground-based DARE Prototype Nhan et al. (in prep.) Polarimeter will 1. Measure polarization leakage caused by ν- dependence of power patterns of linearly polarized dipoles. 2. Further separate polarized foreground from unpolarized 21-cm signal. Full Stokes (I,Q,U) sampling + sky rotation separates polarized sky from unpolarized 21-cm signal 25

18 Detecting the strongest spectral feature in the presence of the Galactic foreground Input theoretical model (Ares) Haslam quiet sky region, constant spectral index. Convolved with ν-dependent Gaussian beam. Ares 21-cm Global Signal model, 3 Turning Points hrs integration with DARE sensitivity. Polynomial fit removed from foreground. Instrument Requirement: Minimize Chromatic beam effects Keith Tauscher & J. Burns 27

19 Signal Extraction using MCMC T C / K ν C ν D / MHz T B / K End-to-end extraction results using EMCEE for DARE instrument C B parameters: 1000 hr, 4 sky regions, DARE beam. B C/D ν B / MHz 1-σ 2-σ C ν C / MHz D ν D ν C / MHz T C This technique captures degeneracies & covariances between parameters, including those related to signal, foregrounds, & the instrument. For details see Harker et al. (2012), MNRAS, 419, 1070; and Harker et al. (2016), MNRAS, 455,

20 Warning against removing higher order polynomials! Harker

21 Characterizing the First Stars & Galaxies Using an MCMC statistical framework, the Galactic foreground is fit along with the physical parameters of the first luminous objects yielding these confidence intervals on physical parameters. Modeling assumes DARE instrument sensitivity. Global Experiments have the potential to bound the properties (e.g., mass, spectra) of the first generation of stars, black holes, & galaxies for the first time ( dex). Mirocha et al

22 Synergies: Major Instruments Planck recently released their full dataset Limit on reionization, nothing about prereionization Hydrogen Epoch of Reionization Array (HERA, PAPER, MWA, LOFAR, etc.) HERA is a next-generation ground-based 21- cm interferometer (Parsons et al.). Should nail down middle/late parts of reionization history May poke into pre-reionization era LEDA, LWA, others may go after very highredshift signal (but ionosphere ) James Webb Space Telescope DARE will have comparable timescale Images (bright) galaxies out to possibly z~15 Athena X-ray probe of black holes/agns to z~10. Behroozi & Silk (2014) JWST Deep Field 31

23 Dark Ages Radio Explorer (DARE) DARE is designed to address: When did the First Stars ignite? What were these First Stars? When did the first accreting Black Holes turn on? What was the characteristic mass? When did Reionization begin? What surprises emerged from the Dark Ages? DARE will accomplish this by: Constructing first sky-averaged spectrum of redshifted 21-cm signal at 11<z<35. Flying spacecraft in lunar orbit & collecting data above lunar farside -- only proven radio-quiet, ionosphere-free zone in inner solar system. Using dipole antennas, in-situ beam measurements & Markov Chain Monte Carlo method to extract spectral turning points in the presence of bright foregrounds. Using high heritage spacecraft bus & technologies/techniques from DARE engineering prototype. DARE will be submitted in response to NASA Explorer AO in Dec Burns et al. 2012, Advances in Space Research, 49,