Probing the reionization process and its sources with Line - - PowerPoint PPT Presentation

Advanced Workshop on Cosmological Structures from Reionization to Galaxies – Trieste, Italy

Probing the reionization process and its sources with Line Intensity Mapping

Marta Silva

Row 1 Row 2 Row 3 Row 4 2 4 6 8 10 12 Column 1 Column 2 Column 3

The high redshift Universe

+ Cross correlating with the 21 cm line

Neutral gas Molecular gas PDRs / Ionized gas / boundary of molecular clouds Recombining gas

HI – 21cm line

Santos et al. 2010 (MNRAS, 46, 2421 )

CO

Gong et al. 2011 (ApJ, 726, L46)

CII

Gong et al. 2011 (ApJ, 745, 49) Silva et al. 2014 (arxiv:1410.4808)

Lyα

Silva et al. 2012 (ApJ, 763, 2) Gong et al. 2014 (ApJ, 785, 72)

Intensity mapping during the EoR

IGM Galaxies

The intensity mapping technique

Line intensity map Galaxies

The simulations: Simfast21 code

21 cm Intensity maps

Halos Ionization Field Non Linear Density Field SFR

Lyα Intensity maps CO Intensity maps CII Intensity maps

Linear Density Field

21 cm Intensity maps

Ionized carbon emission fCII = 1900GHz

(z~8.5 to 5.5) →fo ~ 200–300 GHz

Model and simulating [CII] 157.7 μm emission

CII emission

λCII=157.7 μm Eion(C)=11.26 eV

PDRs IGM Molecular Clouds

UV(6-13.6eV)

HII regions ISM PDRs/Ionized gas

CII intensity: PDRs

DUST

UV(6-13.6e V)

CII

PDR Cooling lines: CII, CI,OI,SiII, FeII

Heating

FIR(1μm-200 μm)

λCII=157.7 μm

Kennicutt (1998) +Cardiel et al. (2003) (Boselli et al. 2002) Local Universe

CII luminosity

HII regions Silva et al. 2014

CII luminosity: PDRs

DUST

UV(6-13.6e V)

CII

PDR Cooling lines: CII, CI,OI,SiII, FeII

Heating

FIR(1μm-200 μm)

λCII=157.7 μm Kennicutt (1998) +Cardiel et al. (2003) (Boselli et al. 2002) Local Universe

CII luminosity

Silva et al. 2014

CII Intensity

HII regions PDR Silva et al. 2014

TIME

(Tomographic Ionized-carbon Mapping Experiment) Wide-band imaging spectrometer using large arrays of direct detectors CII

Gong et al. 2011 (ApJ, 745, 49) Silva et al. 2014 (arxiv:1410.4808)

CII Intensity mapping experiment

21cm/CII cross correlation

freq:200-300 GHz df = 0.4 GHz ang = 1.3 deg δang = 4x10-3 deg Negative correlation

P21,CII = I21 ICII b21 bCII Pδδ

21cm/CII cross correlation

Foregrounds in CII Intensity Maps:

Line emission:

CO(J=2-1),...,CO(J=10-9) OI[145μm], NII[122μm], NII[205μm] and CI[610μm]

Continuum emission:

Stellar emission Free-free Free-bound T wo photon Dust emission Emission from the Milky Way

ν CII≈1900GHz νCO(J=1-0)≈Jx115GHz

Spectraly smooth Spectraly smooth component can be component can be removed along each removed along each line of sight line of sight Yue et all. 2015 Yue et all. 2015 Intensity Intensity smaller smaller than than the CII signal the CII signal Intensity Intensity Larger Larger than the than the CII signall CII signall

CO transitions:

υ(COJ

J-1 →

) ≈ J x 115.271GHz

υ(CII) ≈ 1900GHz

CO contamination in CII intencity maps

Cold gas Helium Hydrogen

CO luminosity

Based in the galaxy catalogs from: Obreschkow et al. 2009b,2009c DeLucia et al. 2006 Molecular Gas/star formation

HI H2 CO

Silva et al. 2014 Gong et al. 2010

CII foregrounds:

Removing CO contamination

Power spectra of CII emission assuming 4 observationally based models

νCII≈1900GHz νCO(J=J-1)≈J х 115GHz

CO(J=2-1),...,CO(J=6-5) <10% Masking freq:200-300 GHz df = 0.4 GHz ang = 1.3 deg δang = 6.67x10-3 deg

Summary

Reionization can be probed with several emission Reionization can be probed with several emission lines ex: 21cm, CO , CII , Ly lines ex: 21cm, CO , CII , Lyα, … α, … Intensity mapping of emission lines may show to be Intensity mapping of emission lines may show to be a more promising tool to study the EoR than a more promising tool to study the EoR than individual observations of galaxies individual observations of galaxies Intensity mapping of several lines can be used to Intensity mapping of several lines can be used to improve constrains on several astrophysical and improve constrains on several astrophysical and cosmological parameters cosmological parameters Cross-correlation of CO, Ly Cross-correlation of CO, Lyα or CII lines and α or CII lines and the 21 the 21 cm linel can help with foregrounds and provide cm linel can help with foregrounds and provide information about the ionization process information about the ionization process