jack burns university of colorado cosmic dawn sigdare signal parameter pipeline: parameter...
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![Page 1: Jack Burns University of Colorado Cosmic Dawn SIGDARE Signal Parameter Pipeline: Parameter Estimation ๐๐ด, ๐,๐= ๐21 (๐ + ๐ ๐ฆ (๐๐ธ๐.๐ธ.1 ln๐ฟ๐=โ1](https://reader033.vdocuments.site/reader033/viewer/2022050106/5f441661daebbd2efd0a31c9/html5/thumbnails/1.jpg)
1Surface Telerobotics
Jack BurnsUniversity of ColoradoCosmic Dawn SIG
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2Surface Telerobotics
DARE Project TeamPrincipal Investigator: Jack Burns, University of Colorado BoulderProject Management & Mission Operations: NASA Ames Research Center: B. Hine & J. Bauman Observatory Project Management: Ball Aerospace & Technologies Corp.: W. Purcell & D. NewellScience Co-Investigators:
Robert MacDowall, NASA GSFC, Project ScientistRichard Bradley, NRAO, Deputy Project ScientistJudd Bowman, Arizona State UniversityAnastasia Fialkov, CfASteven Furlanetto, UCLADayton Jones, Space Science Institute, BoulderJustin Kasper, University of MichiganAbraham Loeb, Harvard UniversityRaul Monsalve, ASU & U. ColoradoJordan Mirocha, UCLADavid Rapetti, University of Colorado BoulderEdward Wollack, NASA GSFC
Collaborators:Michael Bicay, NASA AmesAbhirup Datta, University of Colorado BoulderJonathan Pritchard, Imperial CollegeEric Switzer, NASA GSFC
Graduate Students:Bang Nhan, University of ColoradoKeith Tauscher, University of Colorado
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3Surface TeleroboticsAdapted from Pritchard & Loeb, 2010, Phys. Rev. D, 82, 023006
and Mirocha, Harker, & Burns, 2015, ApJ, 813, 11.
The 21-cm Global Signal Reveals the Birth & Characteristics of the First Stars & Galaxies
B: ignition of first stars
โข When did the First Stars ignite?
What were their characteristics?
โข Is there evidence for exotic
physics (e.g. Dark Matterr
decay) in the Dark Ages?
C: heating by first black holes
โข When did the first accreting black
holes turn on? What were their
characteristics?
D: the onset of reionization
โข What was the history of
Reionization in the early Universe?
TB=25xHI
1+z
10
รฆ
รจรงรถ
รธรท
1/2
1-TCMB
TS
รฆ
รจรงรถ
รธรทmKฮด
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4Surface Telerobotics
DARE observational strategy
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5Surface Telerobotics
DARE ObservatoryTwo Year Mission Lifetimeโข ~1000 hrs integration
above lunar farside.โข shielded from Sun.โข 50x 125 km circular,
equatorial orbit.
DARE probes z=11-35with ฮฝ=40-120 MHz
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6Surface Telerobotics
Foregrounds and Beam Chromaticity
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7Surface Telerobotics
Chromaticity: Design Considerations โข Build antenna with low CTE material &
minimize antenna thermal distortions (<10โ) with sunshade.
โข Accurate modeling & measurement before launch.
โข Measure beam on-orbit using frequency tones transmitted from Earth:โข Circularly polarized, PSK modulated carriers
(6) are sent from ground to DARE.โข DARE receives signals as the spacecraft
orbits above near side of the Moon to sweep beam.
โข Carrier levels are measured by DARE every 20 seconds to produce sampled beam cut.
โข A weak signal is also measured on its return trip to the Earth (Moon reflection) to estimate real-time path loss through the ionosphere.
Green Bank Observatory
140-ft antenna
๐๐๐โ๐ =๐2
64๐3 โ1
๐2โ
๐๐ก๐บ๐ก2๐ฟ๐
2๐๐
๐ ๐กโ๐4 = echo power at 140-ft
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8Surface Telerobotics
Polarimeter: Model-independent Foreground
Cosmic Twilight Polarimeter: Ground-based DARE Prototype
Polarimetry Process to measure Foreground1. Measure โpolarization leakageโ caused by ฮฝ-dependence of power patterns of linearly polarized
dipoles. Rotate spacecraft to measure modulated Stokes Q,U2. Harmonic decomposition of modulated Q,U signal, scale to Stokes I, and subtract.
Nhan, Bradley, & Burns, 2017, AJ, submitted, arXiv:1611.06062.
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9Surface Telerobotics
DARE Signal Parameter Pipeline: Parameter Estimation
๐๐ด,๐๐ ๐, ๐ =
๐
๐21 ๐ ๐๐(๐ +
๐
๐๐ ๐ฆ๐ ๐
๐๐๐(๐ ๐ธ๐. ๐ธ. 1
ln ๐ฟ ๐ = โ1
2 ๐ ๐
๐๐ด,๐ท๐
๐ โ๐๐ด,๐๐
๐,๐
๐๐ ๐
2
Eq. E.2
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10Surface Telerobotics
Summary and Conclusionsโข The Global 21-cm Monopole signal is a powerful
tool to explore the first luminous objects in the Universe and their environs at z>10.
โข DARE science instrument: biconical dipole antenna, pilot-tone injection receiver, digital spectrometer, polarimeter.
โข Challenge of observing weak 21-cm signal in presence of bright foreground is addressed via careful measurements of antenna beam & independent measure of foreground via polarimetry.
โข DARE will set meaningful constraints on: Ly-ฮฑ, ionizing, & X-ray backgrounds that will determine if Pop II or Pop III stars dominated the light output for the first galaxies.
โข DARE has been submitted as a mission proposal to NASAโs MIDEX program.