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Overview of Early Science with AMI: Case Studies and Future Plans

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This document outlines the early science initiatives conducted using the Arcminute Microkelvin Imager (AMI), focusing on the case study of Abell 1914. It details the observing strategy, science goals, and early cluster targets, including selection criteria for clusters based on X-ray luminosity and redshift. The document highlights the need for source subtraction and the design of both blind and targeted surveys, while summarizing the planned observing schedule for 2006 and opportunities for guest observers.

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Overview of Early Science with AMI: Case Studies and Future Plans

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  1. Jonathan Zwart jtlz2@mrao.cam.ac.uk Early Science with AMI

  2. Overview • Case Study: Abell 1914 • Observing strategy & science goals • Early cluster targets • Survey plans 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 2

  3. A1914: 228 Hours with Ryle 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 3

  4. A1914: 34 Hours with AMI Long baselines Short baselines (after radio sources removed) 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 4

  5. 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 5

  6. Only7 (/10) antennas • 18 point sources subtracted  Need for source subtraction • astro-ph/0509215 (MNRAS accepted) 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 6

  7. Observing Strategy • Known clusters • Initial blind surveys • Surveys of equatorial fields (need LA) • Joint fields (AMiBA, SZA, UKIDSS…) 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 7

  8. Early Cluster Targets • Abell (optical) & NORAS (X-ray) • MACS (X-ray, Ebeling et al. 2000) • High-z candidates Ryle source survey (2004–): 4 days for each of ~ 100 ‘lucky’ targets 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 8

  9. NORAS-Selected Clusters Selection criteria: • LX > 6.8×1044 erg s-1 • z > 0.1 • Calibrate scaling relations L–T, M, etc +X-ray g,H0 A263: 10 hours; z = 0.3; (Natasha Hurley-Walker) 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 9

  10. MACS-Selected Clusters Selection criteria: • LX > 1045 erg s-1 • z > 0.5 • Evolution of scaling relations with z +X-ray g (z),H0, q0 MACS 0717+37: 8 hours; z = 0.545 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 10

  11. Blind Surveys • ‘Wedding cake’: • 10 □° deep survey (1 year) • 100 □° shallow survey (6 months) • Evolution of cluster population, N(m,z) • Some experimenting with z from SZ alone • But for now obtain redshifts independently… 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 11

  12. Deep Survey – Optical Fields • ~ 10 sq. deg. on CFHT • R = 24.5, z’ = 23.5 (AB) • WFCAM K = 21.0 (AB) • Clusters out to z ~ 1.5 • Feedback on SZ selection function • Red Cluster Sequence (e.g. Gladders & Yee) • Voronoi tessellation (Culverhouse) • Full Bayesian analysis (Zwart & Hobson) • Spectroscopy 0.96° 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 12

  13. Other Science • CMB power spectrum at high angular scales (ℓ > 3000, cf VSA) • Other non-Gaussian features, e.g. cosmic strings, ionization regions 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 13

  14. Summary • AMI has started obs of known clusters (astro-ph/0509215) • Shallow blind survey of optical fields begins summer 2006 • Deep survey as soon as LA commissioned • Open to guest observers 19 March 2006 Jonathan Zwart, Cavendish Astrophysics 14

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