The CO Mapping Array Pathfinder (COMAP)

Transcription

1 The CO Mapping Array Pathfinder (COMAP) Kieran Cleary (Caltech) AME Workshop, June 3, 06

2 and ERO sources. source L CO( ) /L CO( 0) L CO(3 ) /L CO( 0) L CO(4 3) /L CO( 0) L CO(5 4) /L CO( 0) Aim: QSO CSG M What is COMAP? ultimately, to trace LSS at EoR. In short term, focus on lower-redshift science Gao & Solomon (004) Carilli & Walter (03) Fig. a CO Common star-formation tracer at low redshift Bright, even at high z Traces photon sources responsible for the ionization Emits SMG in line ladder Mapping Intensity mapping: Fig. b aggregate Measure line emission from unresolved galaxies spectra: trace evolution with redshift - tomography Array Single-dish, All-sky, Figure : Redshifted frequencies νobs of CO tracers of the starforming ISM (right) as a νobs = νrest /( + z). The shaded areas indic by various telescopes. Highlighted are the ALM high frequency bands of the JVLA. The color high redshift (z> ) lines. The color of the p types, as explained in the left panel. Fig.. (a) Correlation between HCN and IR luminosities in 65 galaxies. Some limits in HCN luminosities are indicated with arrows. (b) Correlation between LCO and LIR for the same HCN sample. The sample is divided into luminous infrared galaxies (LIGs) and ultraluminous infrared galaxies (ULIGs) with LIR! L" and less luminous normal spiral galaxies. The solid lines are the fits to the less luminous galaxies with a slope fixed at unity. A single slope fits HCN data for both low and high IR luminosities, but not for the CO data. focal-plane array 00-element arrays, broadband backends ultimately required Pathfinder Observed frequency <-> distance Test technology and focus on intermediate redshift, z~-3.

3 COMAP collaboration K. Cleary (PI) Tony Readhead Tim Pearson James Lamb David Woody Sarah Church Risa Wechsler Tony Li Dongwoo Chung Todd Gaier Charles Lawrence Brandon Hensley Clive Dickinson Stuart Harper Andrew Harris Joshua Gundersen Hans Kristian Eriksen Ingunn Wehus 3

4 COMAP Phase I X$ X$ COMAP Phase I BY$ Y$ 6-34 GHz Focal-plane array 9 single-pol pixels m telescope NSF AAG NSF MRI Observe for years m telescope at OVRO COMAP 9 x 8 GHz backend CASPER-based 4

5 COMAP Phase I X$ X$ COMAP Phase I BY$ Y$ 6-34 GHz Focal-plane array 9 single-pol pixels COMAP m telescope NSF AAG NSF MRI Observe for years m telescope at OVRO 9 x 8 GHz backend CASPER-based 5

6 COMAP LNA modules Noise&Temperature&(K)& 30.0# 5.0# 0.0# 5.0#.0# 5.0# 0.0# 6# 8# 30# 3# 34# Freqency&(GHz)& 40 LNA modules already built (JPL R&TD) Using existing MMIC LNA designs (0 nm) Evaluating new 35 nm designs (< K noise from 6-34 GHz noise) Nominal Tsys=44 K (assumes 6 K amplifier noise) 36# 38# 40#

7 Experiment Parameters COMAP Parameters Angular resolution (arcmin) ~4 Number of pixels 9 System temperature (K) 44 Frequency coverage (GHz) Spectral resolution (R) ~800 Final map sensitivity per 4 GHz band in single field (μk).33 -Four fields, each.5 sq deg -,000 hrs observing -Chosen to overlap with galaxy surveys, e.g. COSMOS, DES 7

8 Phase I sensitivity Tony Li COMAP m 6-30 GHz CO(-0) z P (k ) 0 Fiducial Pullen+03, B Righi+008 Pullen+03, A Visbal+Loeb 0 k [Mpc 0 ] Fiducial Righi+008 (approx.) Visbal+Loeb 0 Pullen+03, A Pullen+03, B (approx.) 6-30 GHz CO(-0) z P (k )/ k 3 P (k )/ [µk ] COMAP m (detection significance) k [Mpc 0 ] Single 4-GHz band 8

9 Phase I sensitivity Tony Li COMAP m 6-30 GHz CO(-0) z P (k ) 5 0 Fiducial Pullen+03, B Righi+008 Pullen+03, A Visbal+Loeb 0 k [Mpc 0 ] Fiducial Righi+008 (approx.) Visbal+Loeb 0 Pullen+03, A Pullen+03, B (approx.) 6-30 GHz CO(-0) z Keating et al. P (k )/ k 3 P (k )/ [µk ] COMAP m (detection significance) k [Mpc 0 ] Single 4-GHz band 9

10 Phase II COMAP Phase II 6-34 GHz Focal-plane array 9 single-pol pixels 6-34 GHz Focal-plane array 9 single-pol pixels 6-34 GHz Focal-plane array 9 single-pol pixels 6-34 GHz Focal-plane array 9 single-pol pixels 6-34 GHz Focal-plane array 9 single-pol pixels m telescope m telescope m telescope m telescope m telescope Observe for 3 years 4 GHz backend 5xm telescope at OVRO

11 Phase II sensitivity Tony Li COMAP m: x5 dishes GHz CO(-0) z.4.8 P (k ) 0 Fiducial Pullen+03, B Righi+008 Pullen+03, A Visbal+Loeb 0 k [Mpc 0 ] Fiducial Righi+008 (approx.) Visbal+Loeb 0 Pullen+03, A Pullen+03, B (approx.) GHz CO(-0) z P (k )/ k 3 P (k )/ [µk ] COMAP m: x5 dishes (detection significance) Tony Li k [Mpc 0 ] COMAP Phase II

12 COMAP Phase III COMAP Phase I 6-34 GHz Focal-plane array 9 single-pol pixels m telescope Ka NSF AAG COMAP Ku Observe for years m telescope at OVRO NSF MRI COMAP 9 x 8 Ka GHz backend CASPER-based

13 Foregrounds Foreground Foreground Continuum foregrounds Galactic synchrotron from the Global Sky model (de Oliveira-Costa et al. 008). Free-Free emission from the Planck Sky Model (Delabrouille 03) Point sources (PSM model with limit between strong and faint sources = 0 mjy) CMB (Commander-Ruler CMB intensity map) Galactic synchrotron Free-free Mollview projection Sky at 30 GHz Galactic free-free CMB Synchrotron Point sources Faint point sources CMB Foreground continuua fitted out as loworder modes Line Other HCN foregrounds K_CMB 3 lines redshifted into 6-34 GHz band (-0), CN (-0), CS (-0), HCO+ Brightest line foreground sub-dominant 3

14 Foregrounds model A 6 Continuum foregrounds 5 3 (k ) (µk ) Free-free CMB Synchrotron sources Foreground continua fitted out as low-order modes Line Other HCN foregrounds lines redshifted into 6-34 GHz band (-0), CN (-0), CS (-0), HCO+ Brightest 0 line foreground sub-dominant Figure 5: 3D spherically-averaged power spectra (lef 3 C` over all frequency (right panels), for va channels ity models. Median spectrum values and 95% interv 0 for each model, withlog-space residuals between un 0 taminated CO spectra shown below each spectra plo (CO+HCN)/CO Point CO HCN CO + HCN 4 0 k (Mpc ) Dongwoo Chung 4

15 AME Science Mapping of extended areas: - Galactic: NCP, compact targets - Nearby galaxies MHz spectral resolution (higher possible?) COMAP Parameters Angular resolution (arcmin) ~4 Number of pixels 9 System temperature (K) 44 Frequency coverage (GHz) Spectral resolution (R) ~800 Final map sensitivity per 4 GHz band in single field (μk).33 5

16 Schedule COMAP Phase I fully funded by NSF (AAG + MRI), KISS, Caltech, Stanford, JPL, Miami, Manchester, Oslo 4-year project: -year build, -year observation Start observing October 07!