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From Dark to Light Hydrogen and the First Stars
Tabitha Voytek, Carnegie Mellon University
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SCI-HI Project Collaborators: Jeff Peterson (CMU), Aravind Natarajan (CMU/Pitt) *Omar Lopez-Cruz (INAOE), Jose-Miguel Jauegui-Garcia (INAOE), Edgar Castillo (INAOE) *Other future collaborators in Mexico
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Background
Instrument
Deployment
Analysis
Results
Improvements
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Observations with the SCI-HI experiment focus on first star formation during the Cosmic Dawn.
Image: http://www.nasa.gov/mission_pages/planck/multimedia/pia16876b.html
SCI-HI Observations
3 Background Deployments Results
Instrument Analysis Improvements
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All 21-cm observations are made using Hyperfine splitting of the ground state of hydrogen.
1s 1S1/2
ΔE → 1420 MHz → 21-cm
5 Background Deployments Results
Instrument Analysis Improvements
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Hyperfine splitting is energy differentiation caused by the spin alignment of the proton and electron.
Image from: http://aliceingalaxyland.blogspot.com/2009/04/mini-spinni-antics-of-atoms-in-space.html
6 Background Deployments Results
Instrument Analysis Improvements
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Neutral hydrogen (HI) gas can be found in the Interstellar and Intergalactic Medium (IGM).
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Hydrogen 21-cm Emission Contours for M51
Image from: http://www.haydenplanetarium.org
Background Deployments Results
Instrument Analysis Improvements
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All-sky 21-cm spectrum experiments measure the average redshift evolution of HI gas in the IGM.
Image: Pritchard and Loeb, Nature, 2010
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2/1)1)(1( zTs
initial
T
T
spaceb
Background Deployments Results
Instrument Analysis Improvements
obs
obsemitz
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In particular, the SCI-HI experiment focuses on the all-sky averaged signal during the Cosmic Dawn (z~20).
Image: Pritchard and Loeb, Nature, 2010
9 Background Deployments Results
Instrument Analysis Improvements
SCI-HI Measures Here
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Three primary components were considered in designing the SCI-HI instrument.
Antenna Working Frequencies: 40-130 MHz
RF Electronics Switch, amplifiers, filters and cables
Computer Analog to Digital Conversion and Fourier Transform
11 Background Deployments Results
Instrument Analysis Improvements
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The SCI-HI antenna went through several different iterations before settling on the HIbiscus design.
Trombone Antenna HIbiscus Antenna v1 HIbiscus Antenna v2
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Instrument Analysis Improvements
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Data was collected with the preliminary SCI-HI instrument in June 2013 on Isla Guadalupe.
13 Background Deployments Results
Instrument Analysis Improvements
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At the time, the instrument had a single antenna and relied on 12V car batteries for DC power.
14 Background Deployments Results
Instrument Analysis Improvements
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Terrestrial radio frequency interference (RFI) is a significant problem in radio astronomy.
16 Background Deployments Results
Instrument Analysis Improvements
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We evaluated current and potential experiment sites for their RFI environmental quality.
17 Background Deployments Results
Instrument Analysis Improvements
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At each site, quality was investigated using a portable antenna and spectrum analyzer.
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Algonquin Guadalupe
Background Deployments Results
Instrument Analysis Improvements
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We chose to deploy SCI-HI at Isla Guadalupe based upon the excellent RFI environment.
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FM band as measured with the SCI-HI instrument
Background Deployments Results
Instrument Analysis Improvements
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Data collection includes both the sky signal and calibration source signals.
21 Background Deployments Results
Instrument Analysis Improvements
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Sky signals collected with the HIbiscus antenna are dominated by the Milky Way Galaxy.
22 Background Deployments Results
Instrument Analysis Improvements
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This Milky Way Galaxy signal varies over each day due to the antenna beam sky coverage.
Daily Signal Variation at 70 MHz
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Instrument Analysis Improvements
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Calibration utilizes the Milky Way Galaxy foreground model and daily mean/variance.
Beam Averaged Sky Temperature:
𝑇𝐺𝑆𝑀 𝑡, 𝜐 = 𝑑Ω 𝐺𝑆𝑀 𝜃, 𝜙, 𝜐 𝐵(𝜃 − 𝜃0 𝑡 , 𝜙 − 𝜙0 𝑡 , 𝜐)
𝑑Ω 𝐵(𝜃 − 𝜃0 𝑡 , 𝜙 − 𝜙0 𝑡 , 𝜐)
GSM Model comes from de Oliveira-Costa et al. (2008)
χ² Fitting:
𝜒2 𝜐 = Δ𝑇𝑚𝑒𝑎𝑠 𝑡, 𝜐 − Δ𝑇𝐺𝑆𝑀 𝑡, 𝜐2
𝑡
Daily Mean Subtraction:
Δ𝑇𝑚𝑒𝑎𝑠 𝑡, 𝜐 = 𝑇𝑚𝑒𝑎𝑠 𝑡, 𝜈 − 𝑇𝑚𝑒𝑎𝑠 𝐷𝐴𝑌(𝜐)
Δ𝑇𝐺𝑆𝑀 𝑡, 𝜐 = 𝑇𝐺𝑆𝑀 𝑡, 𝜈 − 𝑇𝐺𝑆𝑀 𝐷𝐴𝑌(𝜐)
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Instrument Analysis Improvements
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KΔGSM calibration is most successful when a full day of data is collected.
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Instrument Analysis Improvements
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Example KΔGSM Mean and Fit
After calibration, foreground removal was done using a simple polynomial fitting and subtraction.
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𝑙𝑜𝑔10 𝑇𝐺𝑀(𝜐) = 𝑎𝑘 𝑙𝑜𝑔10(𝜐
70 𝑀𝐻𝑧)𝑘
𝑛
𝑘=0
𝑇𝑟𝑒𝑠 𝜐 = 𝑇𝑚𝑒𝑎𝑠 𝐷𝐴𝑌 𝜐 − 𝑇𝐺𝑀(𝜐)
Daily Fit:
Daily Residuals:
Background Deployments Results
Instrument Analysis Improvements
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Preliminary data collection in June 2013 gave good results, but further improvements are necessary.
KJNC Calibrated
KΔGSM Calibrated
Predicted 21-cm Signal Models
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Instrument Analysis Improvements
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Problem: DC battery is unreliable. Solution: Replace battery with an AC gas generator.
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Instrument Analysis Improvements
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Problem: DC battery is unreliable. Solution: Replace battery with an AC gas generator.
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Instrument Analysis Improvements
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Problem: Antenna frequency range is too small. Solution: Build multiple scaled antennae.
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70 MHz Scale
100 MHz Scale
Background Deployments Results
Instrument Analysis Improvements
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Problem: Self-generated RFI seen in data. Solution: Double Faraday cage for computer.
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Double Faraday Cage
Computer inside inner Faraday Cage
Background Deployments Results
Instrument Analysis Improvements
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Problem: Isla Guadalupe still not remote enough. Solution: Find more remote sites.
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Time Series of the FM band for June 1st, 2013 data
Time Average of the FM band for June 1st, 2013
Background Deployments Results
Instrument Analysis Improvements
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Problem: Isla Guadalupe still not remote enough. Solution: Isla Socorro/Clarion and/or Marion Island.
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Guadalupe
Socorro Clarion
Marion Island
Background Deployments Results
Instrument Analysis Improvements
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With these changes, the SCI-HI experiment will help us better understand the first stars.
Foregrounds
Current Best Results (KΔGSM)
Predicted 21-cm Models
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Instrument Analysis Improvements
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S C I – H I Sonda Cosmológica de las Islas para la Detección de Hidrógeno Neutro
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