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AzTEC observations of the SZE at 1.1mm & resolving point-source contamination

AzTEC observations of the SZE at 1.1mm & resolving point-source contamination. David Hughes & AzTEC team INAOE, Mexico (LMT Project Scientist). Bullet Cluster at 1.1mm 30 arcsec AzTEC/ASTE beam AzTEC Cluster Evolution Survey (ACES). AzTEC P.I. Grant Wilson (UMASS).

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AzTEC observations of the SZE at 1.1mm & resolving point-source contamination

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  1. AzTEC observations of the SZE at 1.1mm & resolving point-source contamination David Hughes & AzTEC team INAOE, Mexico (LMT Project Scientist) Bullet Cluster at 1.1mm 30 arcsec AzTEC/ASTE beam AzTEC Cluster Evolution Survey (ACES) AzTEC P.I. Grant Wilson (UMASS)

  2. Arcmin-resolution detections of the Sunyaev-Zeldovich effect Wide –area mm-wavelength SZE surveys (100- 40000 sq. degs) detecting ~100 – 1000’s clusters ACT & SPT 2 – 1.1mm; 1- 2 arcminute beam Planck 350um - 1cm; 5 - 33 arcminute beam linear-regime non-linear regime 1 deg 5 arcmin Bullet Cluster - ACBAR map Gomez et al. 2005 beam FWHM ~ 4.5 arcmins

  3. First resolved submillimeter detection of SZE RX J1347-1145 at z~0.45 Submm (JCMT) & Xray (Chandra) contours Komatsu et al. 1999, ApJ, 516, L1

  4. Large Millimeter Telescope (LMT / GTM) • Bi-national project: INAOE (Mexico) & UMASS (USA) • 50-m main reflector (180 panel segments) • active surface (compensates gravity & thermal deformations) to achieve surface r.m.s. of ~70 microns • operational wavelengths 0.85 - 4 mm beam resolution (FWHM) 5 -18 arcsec • FOV ~ 4 arcmin diameter • First-light science starting early 2010 (with inner 32-m diameter)

  5. Volcán Sierra La Negra (97o 18’ 53” W, +18o 59’ 06”) • altitude 4600m

  6. Simulated pt-source contamination from SMGs of the SZE SZE + noise 15 arcmin Cluster mass ~1e15 Msun; core radius ~30 arcsecs; z=0.3 lensed SMG population >0.1mJy at 1.1mm (weak-lensing only - mag < 2) (Austermann etal 2009 + EBL 20 Jy/sq. deg) rms ~0.7mJy/beam (beam ~30 arcsec FWHM; e.g. AzTEC on 10-m ASTE)

  7. Simulated pt-source contamination from SMGs of the SZE SZE + noise SZE + lensed SMGs + noise 9 arcmin Cluster mass ~1e15 Msun; core radius ~30 arcsecs; z=0.3 lensed SMG population >0.1mJy at 1.1mm (weak-lensing only - mag < 2) (Austermann etal 2009 + EBL 20 Jy/sq. deg) rms ~0.7mJy/beam (30 arcsec FWHM; e.g. AzTEC on 10-m ASTE)

  8. AzTEC Cluster Evolution Survey (ACES) ASTE – 10m 2007-2008 LMT – 50m > 2010 JCMT – 15m 2005 40 low-z clusters, intermediate-z & high-z AGN & over-densities (.e.g. LBGs, LAE, ..) between z~0.1 – 6 (>200 sq. arcmins/field, σ ~0.7mJy ) • AzTEC mapping speed at 1.1mm • JCMT: 23-28 arcmin2/mJy2/hr (19 arcsec beam) • ASTE: 20-30 arcmin2/mJy2/hr (27 arcsec beam) • LMT (projected): 1000 arcmin2/mJy2/hr (5 arcsec beam)

  9. MS0451-03 ACES survey: RX J1347-1145 ASTE JCMT SCUBA 345GHz map - offset (Komatsu et al 1999) AzTEC 270 GHz ASTE 30 arcsec beam, rms ~ 0.7 mJy JCMT 18 arcsec beam

  10. Abell 2163 (z=0.203) AzTEC/ASTE 270 GHz full map (400 sq. arcmins) optimised for pt-source for pt source extraction. Currently developing algorithms for maximising extended SZE increment Laboca/APEX 345 GHz Nord et al. 2009, astroph/0902213

  11. Abell 2163 (z=0.203) BCG BCG 12 arcmins AzTEC/ASTE 270 GHz 30 arcsec beam (in prep) Laboca/APEX 345 GHz, 20 arcsec beam Nord et al. 2009, astroph/0902213

  12. Point-source (SMG) contamination of the SZE SPT 2mm APEX-SZ 2mm ASTE – AZTEC 1.1mm 85 arcsec beam 30 arcsec beam 60 arcsec beam 12 mJy pt-source + SZ ~ 3 mJy/beam Impact on estimates of cosmological parameters via SZE still to be determined. Higher resolution LMT, ALMA, … observations will address this. ? 4 arcmins Wilson, G. et al 2008 MNRAS 390, 1061

  13. HST/IRAC counterparts of MMJ0659-5557 critical magnification line 20 arcsecs Most likely interpretation – SMG is a LIRG L<1011 – 1012 L (SFR ~5-50 M/yr) Wilson et al (2008) Lens model of Gonzalez et al. (2008)suggestsamplification ~30 at position of SMG IRAC photo-z z = 2.7+/- 0.2 Wilson et al. 2008 Sub-mm 250-1100um photo-z z = 2.9 (+0.6,-0.3) Rex et al. 2009 (in prep)

  14. scatter in cluster scaling-relations • Still not clear how cluster scaling relations & • determination of cosmological parameters • from SZE will be affected by pt-source • contamination • simulations suggest >= 30% of increment • from high surface-density of faint SMGs • even without SL • less effect in decrement (SMG • spectral-index – fainter but larger beam • convolves more pt-sources) • SZE morphology also affected – • variance in pt. source contamination can be • misinterpreted as temperature substructure • (in core & at large (virial) radii) integrated Y – M relation SZA observations 31GHz 0.2 mJy/beam Marrone et al. astroph – 9 July 2009 measured within 350kpc radius core – 80 arcsec radius at z ~0.3

  15. Future SZE cluster & pt-source observations with LMT (>2010) • AzTEC – 144 pixel 1.1mm camera • SPEED – 4 pixel FSB prototype array (0.8, 1.1, 1.4, 2.1mm) ~1mJy/Hz^1/2 • CIX – 8 x 8 (4-colour) FSB array • TolTEC - large format monolithic 1.1mm array (e.g. SCUBA, MBAC, MUSTANG, ...) ~ 5000 pixels/FOV 3-10 deg^2/hr/mJy^2 • Redshift receiver – 75 – 110GHz dual-pixel dual pol. spectrometer (dnu~35 GHz)

  16. Summary: • sub-mm point-sources are potentially an important contaminant of SZE • nature of pt-sources unclear – • low-z cluster members; high-z SMGs lensed (SL+WL) by cluster members; rare projection of instrinsically luminous SMGs (>HLIRGs); …. ? • higher resolution experiments (<< 10 arcsecs e.g. LMT, ALMA, …..) required to provide pt-source “masks” to clean SZE images of lower resolution experiments (SPT, ACT, Planck ..) • sensitivity & high-resoltuion masks important for higher-z, lower-Y (M) clusters

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