Probing Cosmic Origins with CO and [CII] Emission Lines

Size: px

Start display at page:

Download "Probing Cosmic Origins with CO and [CII] Emission Lines"

Dwight Williamson
5 years ago
Views:

1 Probing Cosmic Origins with CO and [CII] Emission Lines Azadeh Moradinezhad Dizgah A. Moradinezhad Dizgah, G. Keating, A. Fialkov arxiv: A. Moradinezhad Dizgah, G. Keating, A. Fialkov (in prep) Aspen, Cosmological Signals from Cosmic Dawn to the Present, Feb 6th,

2 Inflation Phase of accelerated expansion Classical dynamics: large scale homogeneity and isotropy Quantum fluctuations: primordial perturbations reheating Prediction of the simplest models adiabatic, nearly scale-invariant and Gaussian 2

3 Primordial non-gaussianity h (k 1 ) (k 2 ) (k 3 )i =(2 ) 3 D(k 123 )B (k 1,k 2,k 3 ) B (k 1,k 2,k 3 ) f NL S(k 1,k 2,k 3 ) Amplitude Shape Local Shape: sensitive probe of multi-field inflation single-field consistency relation Maldacena 2003, Creminelli & Zaldarriaga (2004) f loc NL 1 3

4 Observational Constraints Current best limit: CMB by Planck NL) ' 6.5 Future: LSS surveys, in principle, many more modes (3D map) more information LSS: Clustering statistics of biased tracers: Galaxy Surveys (resolve individual sources) Line Intensity Mapping (cumulative light from ensemble of sources) 4 Power Spectrum

5 Scale-dependent Bias h(k, z) =b(z) m (k, z) Dalal, Doré, Huterer & Shirokov (2007) b(z)+ b(k, z) Local PNG: = G f loc NL( 2 G h 2 Gi) b / 1 k 2 Matarrese & Verde (2008), Afshordi & Tolly (2008) 5

Prospects for Redshift Surveys First LSS Constraints: SDSS power spectrum Slosar et al (2008) fnl loc = 28 +23 24 fnl loc =8 +26 37 All Quasars EUCLID:

6 Prospects for Redshift Surveys First LSS Constraints: SDSS power spectrum Slosar et al (2008) fnl loc = fnl loc = All Quasars EUCLID: Moradinezhad Dizgah et al (2018) NL) 3.3 NL) D Power spectrum 3D Bispectrum SPHEREx: Dore et al (2014) NL) 0.8 NL) 0.2 3D Power spectrum 3D Bispectrum 6

7 Ultra Large Scales with Intensity Mapping LIM 2017 Status Report, Kovetz et al. 7

8 PNG with Line Intensity Mapping Constraints on local PNG from IM with 21-cm line 7 <z<8 NL) 10 Joudaki et al (2011) 1 <z<5 NL) 1 Camera et al (2013) Other lines: consider CO and [CII] Small scales: individual star-forming galaxies Large scales: distribution of star-forming galaxies Tentative detection Keating et al (2016), Pullen et al (2017) 8

9 Line Power Spectrum Under the assumption that line emission arise primarily within galaxy host halos: ht line i(z) = c 2 2k B 2 obs Z dm dn dm L(M,z) 4 D 2 L dl d 2 dl d, Fluctuations induced by clustering of matter P clust (k, z) =[ht line i(z)] 2 b 2 line(z)p 0 (k, z) Local PNG: b line (z)! b line (k, z) =b line (z)+ 6 5 f loc NL c (b line (z) 1) M(k, z) 9

10 Survey Design CO(1-0) Ground-based COMAP-Low 10 m aperture 1000 dual-polarization detectors Spectral resolution 30 MHz with coverage of GHz. (3.8<z<8.6) Sky coverage: 2000 sq. deg [CII] Space-based, PIXIE Frequency range of 30 GHz - 6 THz, 400 frequency channels with bandwidth of 15 GHz. [ GHz (0.06 < z < 11.7)] Full-sky coverage, cleanest 75% P N (k, µ) =P N exp[(k /k,res ) 2 +(k? /k?,res ) 2 ] Lidz et al (2011) P N = 2 voxv vox = T 2 sys tot N det surv 10 dl d 2 dl d, COMAP

11 Fisher Forecast Redshift-space distortions Jackson (1972) Kaiser (1987) P s cluster(k, µ, z) =P cluster (k, z) 1+µ 2 (k, z) 2 exp k 2 µ 2 2 v H 2 (z) Alcock-Paczynski effect Alcock and Paczynski (1979), Ballinger et al (1996) P s cluster( k, µ, z) = H true(z) H ref (z) apple DA,ref (z) D A,true (z) 2 P s cluster(k, µ, z) = [ln(10 10 A s ),n s,h, cdm, b,f loc NL, FoG,0] 11

12 Spherically-averaged Power Spectrum 10 5 CO (1 0) at z ' [CII] at z ' 2 P (k) [µk 2 h 3 Mpc 3 ] P clust,f loc NL =6.5 P clust,f loc NL =1 P G P shot k [h 1 Mpc] k [h 1 Mpc] Moradinezhad Dizgah, Keating, Fialkov (2018) 12

13 Results CO(1-0), COMAP-Low: [CII], PIXIE: NL) =3.7 NL) =4.9 z CO, CV CII, CV CO, COMAP CII, PIXIE (f NL loc ) z 13

14 Conclusions Intensity mapping is a powerful technique to probe cosmology Access to very large scales and high redshifts at much lower cost Achieve (f NL )=O(1) with partial sky-coverage Further Improvements: Multi-tracer technique McDonald & Seljak (2008), Seljak (2009) Line bispectrum 14

SEARCHING FOR LOCAL CUBIC- ORDER NON-GAUSSIANITY WITH GALAXY CLUSTERING

SEARCHING FOR LOCAL CUBIC- ORDER NON-GAUSSIANITY WITH GALAXY CLUSTERING Vincent Desjacques ITP Zurich with: Nico Hamaus (Zurich), Uros Seljak (Berkeley/Zurich) Horiba 2010 cosmology conference, Tokyo,