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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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slide1

Probing the Epoch of Reionization

with the

TomographicIonized-carbon

Mapping Experiment (TIME)

Jamie Bock

Caltech / JPL

CCAT Workshop, Boulder CO

21 September 2012

slide5

Relationship Between Dark Matter and Galaxies

Halo Clustering Model

Cooray &

Sheth 2002

slide7

Spatial Power Spectrum of SPIRE Maps

2-halo clustering

1-halo clustering

Viero et al. arXiv 1208.5049

slide8

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!
slide9

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

slide10

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

slide11

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
slide12

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
slide13

CO vs C+

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

slide14

CO Foreground Contamination?

Gong et al. 2012, ApJ 745, 49G

slide16

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

slide17

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

slide18

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
slide19

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!

slide20

SuperSpec: 80-Channel Test Device

7 mm

Erik Shirokoff, chip design

slide21

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

slide22

Low-NEP TES Bolometers

Work with SQUID TD Mux

slide23

Power Spectra in 3 Bands

Viero et al. arXiv 1208.5049

slide24

Inverted microstrip stack

Erik Shirokoff, SuperSpec chip design

high redshift galaxies in hermes 500 um peaked sources

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

slide26

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