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Probing the Epoch of Reionization with the T omographic I onized-carbon

Probing the Epoch of Reionization with the T omographic I onized-carbon M apping E xperiment (TIME) Jamie Bock Caltech / JPL CCAT Workshop, Boulder CO 21 September 2012. Large Scale Structure HerMES Lockman Survey Field. 3.6°. Use Maps to Measure Clustering.

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Probing the Epoch of Reionization with the T omographic I onized-carbon

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  1. Probing the Epoch of Reionization with the TomographicIonized-carbon Mapping Experiment (TIME) Jamie Bock Caltech / JPL CCAT Workshop, Boulder CO 21 September 2012

  2. Large Scale StructureHerMESLockman Survey Field 3.6°

  3. Use Maps to Measure Clustering

  4. An Example of Intensity Mapping

  5. Relationship Between Dark Matter and Galaxies Halo Clustering Model Cooray & Sheth 2002

  6. Large Scale StructureHerMESLockman Survey Field 3.6°

  7. Spatial Power Spectrum of SPIRE Maps 2-halo clustering 1-halo clustering Viero et al. arXiv 1208.5049

  8. Advantages of Intensity Mapping • Measuring to the Galactic Ensemble • Luminosity function • Total photon production • Large-scale structure • Science Applications • Galaxy evolution • Link between dark matter and galaxy formation • Epoch of Reionization? • Baryon Acoustic Oscillations? • Observationally Expedient • Does not require a large telescope!

  9. kSZ and Galaxies: SPIRE & mm-wave Precise Measures of kSZ and tSZ SPT Herschel/SPIRE 250 um 350 um Correlate FIR galaxies with CMB lensing projected potential: CMB lensing x CIB 500 um

  10. Near-IR Fluctuations from the EOR? Kashlinsky et al. 2005 3.6 um 4.5 um 2p/q [arcsec] 12 x 6 arcmin 10 arcmin Akari 2.4 um 3.2 um 4.1 um Matsumoto et al. 2010

  11. Advantages of Line Intensity Mapping • Measuring to the Galactic Ensemble • Luminosity function • Total photon production • Large-scale structure • Science Applications • Galaxy evolution • Link between dark matter and galaxy formation • Epoch of Reionization! • Baryon Acoustic Oscillations! • Observationally Expedient • Does not require a large telescope! • Does require a high-AW spectrometer

  12. C+ Theory Predictions Simulated Sky in C+ Gong, Cooray et al. 2012, ApJ 745, 49G • C+ serves as a tracer of star formation • The clustering signal traces total luminosity • -> unlike a flux-limited galaxy survey • Use C+ to spatially trace SF during the reionization epoch

  13. CO vs C+ CO for EOR studies: Visbal & Loeb 2010, Carilli 2011, Lidz et al. 2011, Gong et al. 2011

  14. CO Foreground Contamination? Gong et al. 2012, ApJ 745, 49G

  15. TIME: Tomographic Ionized-C Mapping Experiment

  16. TIME C+ Sensitivity Predictions Poisson ±1s error in MZ – M relation Clustering Visbal & Loeb D2CO* (104)2 Lidzet al. 2011 D2CO*40002 agrees with Gong C+ model at z = 7 LCII from Visbal & Loeb 10 m Gong et al. 2012, ApJ 745, 49G

  17. Using 21 cm & C+ Together C+ and 21 cm Cross-Correlation 2.5 arcmin • Star formation rate vs. z • Ionization state vs. z • Bubble size Gong et al. 2012, ApJ 745, 49G

  18. TIME-Pilot Sensitivity z = 6 4.5 3.7 • Goals: • Measure C+ fluctuation amplitude • Constrain high-J CO fluctuations by cross-band correlations • Determine atmospheric noise after spectral template subtraction

  19. Filter-Bank Spectrometer • Radiation propagates down main feed line • Resonators respond in narrow bands • Couple to power detector (MKID or TES) Credit: Jonas Zmuidzinas See talk by Matt Bradford later today!

  20. SuperSpec: 80-Channel Test Device 7 mm Erik Shirokoff, chip design

  21. Conclusions EOR Science accessible with a 3-m class dedicated telescope A moderate pilot experiment can probe C+ signal amplitude at lower z Develop new filter-band spectrometer technologies for CCAT

  22. Low-NEP TES Bolometers Work with SQUID TD Mux

  23. Power Spectra in 3 Bands Viero et al. arXiv 1208.5049

  24. Inverted microstrip stack Erik Shirokoff, SuperSpec chip design

  25. Obtain mm-wave redshifts (CO, C+)!! New: Galaxies with Red Colors Are they cold or at high redshift (z=4-7)? 250 um 350 um 500 um * High Redshift Galaxies in HerMES500 um peaked sources APEX ZSPEC: Bolometric spectrometer CSO *Confusion reduced S(500) – fS(250) Red Source AbundanceDowell 2011, in prep. Red Source Case Study Riechers 2011, in prep. PdBI CARMA

  26. Use Clustering to Probe Reionization Spatial Power Spectrum Electromagnetic Spectrum Fit to Spitzer Minimum reionization See Cooray et al. 2004, Kashlinsky 2004 • Why CIBER is Robust to Systematic Errors • Zodiacal Smoothness? Observe at different times of year • Flat Field? Use difference images, lab flat • 1/f noise? Assess using sky differences • Galaxies? Large ℓ separation from EOR • Foregrounds? EOR has very different colors • Anything else? Cross-correlate with Spitzer

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