1. Surveys of high-z galaxies and galaxy clusters with AzTEC Sungeun Kim Sungeun Kim Astronomy & Space Science Department Sejong University Sejong University

2. AzTEC (Astronomical Thermal Emission Camera) Instrument AzTEC is a bolometer camera (designed for imaging) AzTEC is a bolometer camera (designed for imaging) AC voltage output directly proportional to optical power. AC voltage output directly proportional to optical power. Detectors read out continuously at 64Hz. Detectors read out continuously at 64Hz. System designed to have good low freq. stability (AC biased) System designed to have good low freq. stability (AC biased) All commands and signals pass via fiber optics (low flux demands low systematics) All commands and signals pass via fiber optics (low flux demands low systematics) 144 element spiderweb bolo array – S. Golwala

4. AzTEC Collaborators G. Wilson (PI), J. Austermann, K. Scott, T. Perera, G. Wilson (PI), J. Austermann, K. Scott, T. Perera, M. Yun (UMass, USA) M. Yun (UMass, USA) J. Bock, N. Scoville (Caltech, USA) J. Bock, N. Scoville (Caltech, USA) P. Mauskopf (Cardiff, UK) P. Mauskopf (Cardiff, UK) I. Aretxaga, D. Hughes (INAOE, Mexico) I. Aretxaga, D. Hughes (INAOE, Mexico) J. Lowenthal (Smith College, USA) J. Lowenthal (Smith College, USA) E. Chapin, M. Halpern, A. Pope, D. Scott (UBC, Canada) E. Chapin, M. Halpern, A. Pope, D. Scott (UBC, Canada) K. Coppin (University of Durham, UK) K. Coppin (University of Durham, UK) Y. Kang, S. Youn, Y. Kim, K. Kim (Sejong Univ., Korea) Y. Kang, S. Youn, Y. Kim, K. Kim (Sejong Univ., Korea)

5. AzTEC New ‘Science’ detector array 110/144 working detectors (others possibly repairable) Pass band: 1.1 mm, 2.1 mm Raw detector sensitivity: 15mJy Beamsize: 18 arcsec. FWHM Field of View: 4.8 arcmin Jiggle Mapping Speed: 4hrs/FOV/mJy 2 Scan Mapping Speed: 20 arcmin 2 /hr/mJy 2 Continuous JCMT Observing, Nov 10 – Jan 2 > 400 hrs observing time on SMG projects

6. Pre-shipment checkoutOptics alignment at JCMT

7. AzTEC on the JCMT

8. AzTEC New ‘Science’ detector array 110/144 working detectors (others possibly repairable) Pass band: 1.1 mm, 2.1 mm Raw detector sensitivity: 15mJy Beamsize: 18 arcsec. FWHM Field of View: 4.8 arcmin Jiggle Mapping Speed: 4hrs/FOV/mJy 2 Scan Mapping Speed: 20 arcmin 2 /hr/mJy 2 Continuous JCMT Observing, Nov 10 – Jan 2 > 400 hrs observing time on SMG projects

9. Oversized optics minimize microphonic pickup 24bit digitization of signals at cryostat eliminates pickup from long cable runs The opacity at 225 GHz was recorded every 10 minutes by the CSO tau Monitor. The array orientation is fixed in Azimuth and Elevation, the scan-angle in the RA-DEC plane for a raster scan map continuously changes due to sky rotation.

10. AzTEC/JCMT SMG Studies Field Size [arcmin 2 ] Obs Time [hrs] target σ [mJ] PISHADES1800 198.5 (225) 0.7Dunlop COSMOS900 45 (45) 1.0D.Sanders GOODS-N160 43 (90) 0.3E.Chapin MS0451225 30 (30) 0.5I.Smail 4C41.17200 48 (48) 0.3D.Hughes 0316-25750 30 (30) 0.3H.Rottgering BR095221 14.65 (24) 0.8K.Knudsen ~1deg 2

11. Dust emission: far-IR & sub-mm Dusty star-forming galaxies emit much of their light at IR to mm wavelengths Figure from van Kampen (2005) AzTEC is aimed for making a series of confusion-limited surveys of the Submillimeter Galaxies (SMGs), environments of clusters at 1.1 mm wavelength in order to study the dusty starburst populations both in and behind clusters, and blank field.

12. Submillimeter Galaxies Population of extremely luminous high-redshift dust-obscured galaxies detected by their sub-mm and mm wavelength emission. Population of extremely luminous high-redshift dust-obscured galaxies detected by their sub-mm and mm wavelength emission. Massive galaxies, with SFR of ~500-1000 M sun /yr. Sub-mm SCUBA surveys in late 90s (Smail et al 2000, Ivison et al. 98). Massive galaxies, with SFR of ~500-1000 M sun /yr. Sub-mm SCUBA surveys in late 90s (Smail et al 2000, Ivison et al. 98). SMGs: F 850 > 1 mJy. Spectroscopic redshifts for higher redshift population (z~2), median F 850 ~ few mJy for z~2 population. SMGs: F 850 > 1 mJy. Spectroscopic redshifts for higher redshift population (z~2), median F 850 ~ few mJy for z~2 population. Before Spitzer and SHARC-2 observations (Kovacs et al. 2006), mostly 850 micron, some 450 micron, radio observations, CO, and some mm imaging. Before Spitzer and SHARC-2 observations (Kovacs et al. 2006), mostly 850 micron, some 450 micron, radio observations, CO, and some mm imaging. SMM J02399-0136 (Genzel et al. 03) ㅋ =2.5

13. AzTEC bandpass z=1 Submm Galaxies as tracers of structure formation (model SMG spectrum by Efstathiou, Rowan-Robinson and Siebenmorgen, 2000) One of the most exciting developments of the past decade has been the resolution of the cosmic far-infrared background into discrete sources, providing a first glimpse of the rapid build-up of massive galaxies in the early universe long predicted by theory.

14. AzTEC bandpass z=1 z=2 Submm Galaxies as tracers of structure formation (model SMG spectrum by Efstathiou, Rowan-Robinson and Siebenmorgen, 2000) Deep, wide blank-field surveys at mm & sub-mm wavelengths have shown that ultraluminous infrared galaxies (ULIRGs) at z>1, contribute significantly to the Observed far-IR background.

15. AzTEC bandpass z=1 z=2 z=5 Submm Galaxies as tracers of structure formation (model SMG spectrum by Efstathiou, Rowan-Robinson and Siebenmorgen, 2000) Multi-wavelegnth follow-up studies of these so-called sub-mm galaxies (SMGs) suggest that they are massive, young galaxies seen during the period of rapid stellar mass build-up with very high specific star formation rates at z>1. Here are four key questions we would like to address from AzTEC SMG surveys.

16. Scientific Goals of SMG Studies How is the SMG population How is the SMG population distributed in redshift? Are SMG redshift associations Are SMG redshift associations linked to overdensities of other more numerous galaxy classes at the same redshift? Do they reside in such massive Halos? How are SMGs distributed in relation to large scale structure? Overzier et al. (2003) Answering these questions and more will require large confusion limited surveys with multi-spectral follow-up.

17. Galaxy Density Map of COSMOS from Scoville et al. (2007), with the boundaries of the AzTEC, Bolocam, and MAMBO mm surveys (including a massive galaxy cluster at z=0.73) Both MAMBO and BOLOCAM surveys cover a low galaxy density region of the COSMOS field, whilst our new AzTEC observations are designed to examine the impact of massive large- Scale foreground structures on SMG Surveys in order to provide a measure of the importance of cosmic variance in the observed source density at millimeter wavelengths.

18. AzTEC/COSMOS 34 raster-scan Observations, Each centered at (RA,DEC)= (10h00m00s, 02deg36’00’’) 0.3deg 2 region Scan speed of 90”/s-150”/s Mapping speed: 34 arcmin 2 mJy -2 hr -1 (strong function of Sky opacity at 225 GHz)

19. Disadvantages to Chopping sensitive to differential pickup from dish (secondary support, temperature gradients, etc.) resolve out large scale structure Advantages to Rastering beam response stationary on telescope uniform coverage achievable despite incomplete array unlimited sky coverage possible

20. Typical AzTEC Chopped Signal Mean traces out time evolution of atmosphere + variable offsets 2Jy

21. Atmosphere Subtraction with PCA

22. AzTEC/BOLOCAM Comparison Map shows >20% maximum coverage region, with 50% and 75% contours overlaid. Black circles are >3.5 sigma sources, and those in the source catalogue (75% region) are labeled by their number. Purple circles indicate Bolocam sources. Solid purple line marks the Bolocam 1.9 mJy rms contour, dashed line is Bolocam 2.8 mJy rms contour. 2 coincident sources: Bolocam #1 is 3.5 arcsec from AzTEC #1 and Bolocam #13 is 3.6 arcsec from AzTEC #6. Map shows >20% maximum coverage region, with 50% and 75% contours overlaid. Black circles are >3.5 sigma sources, and those in the source catalogue (75% region) are labeled by their number. Purple circles indicate Bolocam sources. Solid purple line marks the Bolocam 1.9 mJy rms contour, dashed line is Bolocam 2.8 mJy rms contour. 2 coincident sources: Bolocam #1 is 3.5 arcsec from AzTEC #1 and Bolocam #13 is 3.6 arcsec from AzTEC #6. Scott et al. (2008)

23. COSMOS Clustering measurement 2-pt angular correlation function made using >2.0 sigma sources. Used a binsize of 36 arcsec, limited to angular separations between 60 and 500 arcsec. No strong clustering signal detected on any scale here. Angular correlation function w( θ ) is projection of the spatial function on the sky and is defined in terms of the joint probability delta P= N 2 [1+w( θ )]d Ὠ 1 Ὠ 2 (N; mean surface density of objects); w=0, distribution is homogeneous. 2-pt angular correlation function made using >2.0 sigma sources. Used a binsize of 36 arcsec, limited to angular separations between 60 and 500 arcsec. No strong clustering signal detected on any scale here. Angular correlation function w( θ ) is projection of the spatial function on the sky and is defined in terms of the joint probability delta P= N 2 [1+w( θ )]d Ὠ 1 Ὠ 2 (N; mean surface density of objects); w=0, distribution is homogeneous.

24. Galaxy Density Map of COSMOS from Scoville et al. (2007), with the boundaries of the AzTEC, Bolocam, and MAMBO mm surveys (including a massive galaxy cluster at z=0.73) from Scoville et al. (2007), with the boundaries of the AzTEC, Bolocam, and MAMBO mm surveys (including a massive galaxy cluster at z=0.73)

25. Cross-Correlation function is computed between the galaxy overdensity map and the AzTEC map No obvious peak at the Center. No obvious peak at the Center. Image Credit: Scott et al. (2006)

26. AzTEC/COSMOS: Conclusion 0.3 deg 2 region imaged within the COSMOS with 1.3 mJy/beam at 1.1mm 0.3 deg 2 region imaged within the COSMOS with 1.3 mJy/beam at 1.1mm 50 sources found S/N>3.5; 16 detected with S/N>4.5, where the number of false-detections is zero; 7 of >5σ sources confirmed with SMA. 50 sources found S/N>3.5; 16 detected with S/N>4.5, where the number of false-detections is zero; 7 of >5σ sources confirmed with SMA. AzTEC sources are spread throughout the field and only 3 are located in z=0.73 cluster environment. AzTEC sources are spread throughout the field and only 3 are located in z=0.73 cluster environment. Our catalogue is 50% complete at an intrinsic flux density of 4 mJy, and 100% is complete at 7 mJy. Our catalogue is 50% complete at an intrinsic flux density of 4 mJy, and 100% is complete at 7 mJy. Fraction of AzTEC sources with potential radio counterparts is 36% and is consistent with that found in SCUBA/SHADES survey (Ivison et al. 2007) at similar fluxes. Fraction of AzTEC sources with potential radio counterparts is 36% and is consistent with that found in SCUBA/SHADES survey (Ivison et al. 2007) at similar fluxes. A detailed comparison of the IRAC color-color plots and SEDs shows that AGNs and SMGs are distinct from each other due to intrinsic differences in their energy source and dust distribution. SMGs as a group have a flatter SED in comparison with AGNs. Only 20% of the objects overlap in the color- color plots and this suggests that SMGs powered by an AGN are not common. In the context of ULIRG-QSO evolutionary senario (Sanders et al. 1988; Norman & Scoville 1988), the little overlap between the AGNs and the SMG population indicates that transition period is much shorter than the duration of the SMG or the IR AGN phase. A detailed comparison of the IRAC color-color plots and SEDs shows that AGNs and SMGs are distinct from each other due to intrinsic differences in their energy source and dust distribution. SMGs as a group have a flatter SED in comparison with AGNs. Only 20% of the objects overlap in the color- color plots and this suggests that SMGs powered by an AGN are not common. In the context of ULIRG-QSO evolutionary senario (Sanders et al. 1988; Norman & Scoville 1988), the little overlap between the AGNs and the SMG population indicates that transition period is much shorter than the duration of the SMG or the IR AGN phase. Estimates of resolved fraction of millimeter CIB due to radio & mid-IR galaxy populations is 7±1% & 21±3% respectively. Estimates of resolved fraction of millimeter CIB due to radio & mid-IR galaxy populations is 7±1% & 21±3% respectively.

27. (a) Empty squares are SMGs securely identified by radio and CO interferometric imaging. Filled squares and pentagons are SMGs identified as “starburst” and “starburst+AGN” by Spitzer IRS spectra, respectively (Menendez-Delmestre et al. 2007; Valiante et al. 2007; Rigby et al. 2008; Pope et al. 2008). IR QSOs with power-law spectrum identified in the FLS field by Lacy et al. and Martinez-Sansigre et al. (2008) are shown as stars. Small dots represent 4000 random field galaxies in the COSMOS field (Sandetrs et al. 2007), and the large circle centered near (-0.4,-0.4) represents the centroid of the IRAC sources in the FLS (Lacy et al. 2004). The long-dashed line outlines the region for AGNs proposed by Lacy et al. The solid line shows the extended region we propose for the identification of SMG counterparts. (b) Filled circles are 9 SMGs identified by direct SMA measurements and empty circles represent the foreground/interloper IRAC sources. (c) Redshift evolution colour-colour tracks for 3 different starburst ages based on theoretical starburst SED models and filled and empty squares along the redshift evolution colour tracks mark the redshifts of z=0.5,1,2,3,4,and 5. The thick solid line represents power-law spectrum sources with s=0.3-1.0. (d) Effects of extinction are demonstrated by the 72 Myr old starburst colour-colour model tracks with total extinction of A V and 200 (Yun et al. 2008). (a) Empty squares are SMGs securely identified by radio and CO interferometric imaging. Filled squares and pentagons are SMGs identified as “starburst” and “starburst+AGN” by Spitzer IRS spectra, respectively (Menendez-Delmestre et al. 2007; Valiante et al. 2007; Rigby et al. 2008; Pope et al. 2008). IR QSOs with power-law spectrum identified in the FLS field by Lacy et al. and Martinez-Sansigre et al. (2008) are shown as stars. Small dots represent 4000 random field galaxies in the COSMOS field (Sandetrs et al. 2007), and the large circle centered near (-0.4,-0.4) represents the centroid of the IRAC sources in the FLS (Lacy et al. 2004). The long-dashed line outlines the region for AGNs proposed by Lacy et al. The solid line shows the extended region we propose for the identification of SMG counterparts. (b) Filled circles are 9 SMGs identified by direct SMA measurements and empty circles represent the foreground/interloper IRAC sources. (c) Redshift evolution colour-colour tracks for 3 different starburst ages based on theoretical starburst SED models and filled and empty squares along the redshift evolution colour tracks mark the redshifts of z=0.5,1,2,3,4,and 5. The thick solid line represents power-law spectrum sources with s=0.3-1.0. (d) Effects of extinction are demonstrated by the 72 Myr old starburst colour-colour model tracks with total extinction of A V =50 and 200 (Yun et al. 2008). Majority of SMGs appear scattered about the model SED colour tracks, consistent with their Spitzer IRS spectra being characteristic of starburst-dominated systems. For a given model SED, the IRAC color becomes monotonically redder with increasing redshift at z>1, and most SMGs have colors consistent with model SEDs redshifted to z=1-5; the weak dependence on extinction A V can be understood since optical depth is greatly reduced at these long wavelengths. As redshift increases, the IRAC bands begin to probe the near-IR to optical bands, and an increasing dependence on extinction is expected. IRAC colors of the two model SEDs diverge at z>2, with the higher extinction A V =200 model predicting redder IRAC colors as expected. Among 50 SMG candidates in COSMOS, 7 AzTEC sources are confirmed with SMA interferometric imaging (Younger et al. 2007). IRAC color-color plots of SMGs are systematically bluer than AGN identification and consistent with 30-70 Myr old starbursts observed at redshifts between z~1 and z~5 (Yun et al. 2008). Figure Credit: Yun et al. (2008)

28. IRAC color-color plot Lacy et al. (2004) from Spitzer FLS. Dashed lines mark “AGN- demarcated region” Lacy et al. (2004) from Spitzer FLS. Dashed lines mark “AGN- demarcated region” Hot dust clustering

29. Spectral Energy Distribution for the Starburst Model τ TdTd SFR Contribution functions & SEDs from Efstathiou (2000). Cartoon by Y. Kim

30. Overall, starbursts age and redshift as the dominant physical parameters affect the observed IRAC colors. SMGs with reddest IRAC colors requires young ( 3) or a power- law AGN dominating the rest frame near-IR SED. Young, dusty starbursts exhibit red IRAC colors, and red IRAC color is not unique to power-law AGNs. The popular AGN identification methods using red IRAC colors, such as by Lacy et al. (2004) and Stern et al. (2005) should be cautious.

31. AzTEC/COSMOS: Conclusion 0.3 deg 2 region imaged within the COSMOS with 1.3 mJy/beam at 1.1mm 0.3 deg 2 region imaged within the COSMOS with 1.3 mJy/beam at 1.1mm 50 sources found S/N>3.5; 16 detected with S/N>4.5, where the number of false- detections is zero; 7 of >5σ sources confirmed with SMA; IRAC color-color plots indicate that SMGs are systematically bluer, consistent with 30 to 70 Myr old starbursts observed at redshifts between z~1 and z~5. 50 sources found S/N>3.5; 16 detected with S/N>4.5, where the number of false- detections is zero; 7 of >5σ sources confirmed with SMA; IRAC color-color plots indicate that SMGs are systematically bluer, consistent with 30 to 70 Myr old starbursts observed at redshifts between z~1 and z~5. AzTEC sources are spread throughout the field and only 3 are located in z=0.73 cluster environment. AzTEC sources are spread throughout the field and only 3 are located in z=0.73 cluster environment. Our catalogue is 50% complete at an intrinsic flux density of 4 mJy, and 100% is complete at 7 mJy. Our catalogue is 50% complete at an intrinsic flux density of 4 mJy, and 100% is complete at 7 mJy. Fraction of AzTEC sources with potential radio counterparts is 36% and is consistent with that found in SCUBA/SHADES survey (Ivison et al. 2007) at similar fluxes. Fraction of AzTEC sources with potential radio counterparts is 36% and is consistent with that found in SCUBA/SHADES survey (Ivison et al. 2007) at similar fluxes. A detailed comparison of the IRAC color-color plots and SEDs shows that AGNs and SMGs are distinct from each other due to intrinsic differences in their energy source and dust distribution. SMGs as a group have a flatter SED in comparison with AGNs. Only 20% of the objects overlap in the color-color plots and this suggests that SMGs powered by an AGN are not common. In the context of ULIRG-QSO evolutionary senario (Sanders et al. 1988; Norman & Scoville 1988), the little overlap between the AGNs and the SMG population indicates that transition period is much shorter than the duration of the SMG or the IR AGN phase. A detailed comparison of the IRAC color-color plots and SEDs shows that AGNs and SMGs are distinct from each other due to intrinsic differences in their energy source and dust distribution. SMGs as a group have a flatter SED in comparison with AGNs. Only 20% of the objects overlap in the color-color plots and this suggests that SMGs powered by an AGN are not common. In the context of ULIRG-QSO evolutionary senario (Sanders et al. 1988; Norman & Scoville 1988), the little overlap between the AGNs and the SMG population indicates that transition period is much shorter than the duration of the SMG or the IR AGN phase. Estimates of resolved fraction of millimeter CIB due to radio & mid-IR galaxy populations is 7±1% & 21±3% respectively. Estimates of resolved fraction of millimeter CIB due to radio & mid-IR galaxy populations is 7±1% & 21±3% respectively.

32. AzTEC/COSMOS: Conclusion 0.15 deg 2 region imaged within the COSMOS with 1.3 mJy/beam at 1.1mm 0.15 deg 2 region imaged within the COSMOS with 1.3 mJy/beam at 1.1mm 50 sources found S/N>3.5; 16 detected with S/N>4.5, where the number of false-detections is zero; 7 of >5σ sources confirmed with SMA. 50 sources found S/N>3.5; 16 detected with S/N>4.5, where the number of false-detections is zero; 7 of >5σ sources confirmed with SMA. AzTEC sources are spread throughout the field and only 3 are located in z=0.73 cluster environment. AzTEC sources are spread throughout the field and only 3 are located in z=0.73 cluster environment. Our catalogue is 50% complete at an intrinsic flux density of 4 mJy, and 100% is complete at 7 mJy. Our catalogue is 50% complete at an intrinsic flux density of 4 mJy, and 100% is complete at 7 mJy. Fraction of AzTEC sources with potential radio counterparts is 36% and is consistent with that found in SCUBA/SHADES survey (Ivison et al. 2007) at similar fluxes. Fraction of AzTEC sources with potential radio counterparts is 36% and is consistent with that found in SCUBA/SHADES survey (Ivison et al. 2007) at similar fluxes. A detailed comparison of the IRAC color-color plots and SEDs shows that AGNs and SMGs are distinct from each other due to intrinsic differences in their energy source and dust distribution. SMGs as a group have a flatter SED in comparison with AGNs. Only 20% of the SMGs overlap in the color- color plots with AGNs and this suggests that SMGs powered by an AGN are not common. In the context of ULIRG-QSO evolutionary senario (Sanders et al. 1988; Norman & Scoville 1988), the little overlap between the AGNs and the SMG population indicates that transition period is much shorter than the duration of the SMG or the IR AGN phase (Yun et al. 2008). A detailed comparison of the IRAC color-color plots and SEDs shows that AGNs and SMGs are distinct from each other due to intrinsic differences in their energy source and dust distribution. SMGs as a group have a flatter SED in comparison with AGNs. Only 20% of the SMGs overlap in the color- color plots with AGNs and this suggests that SMGs powered by an AGN are not common. In the context of ULIRG-QSO evolutionary senario (Sanders et al. 1988; Norman & Scoville 1988), the little overlap between the AGNs and the SMG population indicates that transition period is much shorter than the duration of the SMG or the IR AGN phase (Yun et al. 2008). Estimates of resolved fraction of millimeter CIB due to radio & mid-IR galaxy populations is 7±1% & 21±3% respectively. Estimates of resolved fraction of millimeter CIB due to radio & mid-IR galaxy populations is 7±1% & 21±3% respectively.

33. Summary Remarks We are starting the transition from SMG discovery to SMG study. AzTEC/JCMT is the first step towards developing a census of the SMG population. AzTEC on the Large Millimeter Telescope can systematically sample the faint end of the flux spectrum.

34. LMT/GTM 50m dia. 70um surface 15000 ft alt Sierra Negra, MX

35. Summary Remarks We are starting the transition from SMG discovery to SMG study. AzTEC/JCMT is the first step towards developing a census of the SMG population. Large Millimeter Telescope can systematically sample the faint end of the flux spectrum. Thank you: 감사합니다.

36. Number Counts and Evolution Borys et al. 2003 no evolution

37. Observationally Speaking: SCUBA/JCMT, MAMBO/IRAM 30-m, BOLOCAM/CSO Fewer than100 sources with S/N > 4 Dynamic range: 1-10 mJy at 850 um Severely confusion limited Secure redshifts for only about 20-30 galaxies (controversial!!!) Ivison et al. 2000 Laurent et al. 2005 1.4mJy rms 3σ peaks circled

38. AzTEC Internal Optics Layout Folded optical design minimizes optical microphonic pickup and thermal gradients

40. 42 Jy 2 pW 10 10 photons/s ~1Jy Beam Mapping Products: relative bolometer positions calibration beam shapes

41. 2MASS Z~1500 Z~0.1 THE BIG QUESTION How does structure form and evolve in the Universe? WMAP

42. Hughes et al. 1998 2 arcmin dia. 5 sources > 1mJy (0.05 fW) (300,000 photons/s) AzTEC Array 4.5 arcmin dia. 110 working det. ~15mJy rt(s) sens.

43. Z~1500 Z~0.1 THE BIG QUESTION How does non-linear structure form and evolve in the Universe? SDSS, HST, Chandra … 2MASS Z < few WMAP Epoch of structure formation

44. CMB 2.7K backlight 0.6 pW 3.6×10 9 photons/s Hughes et al. 1998 2 arcmin dia. 5 sources > 1mJy (0.05 fW) (300,000 photons/s)

45. Atmosphere 20-30K foreground 13.7 pW 8×10 10 photons/s Telescope ~30K foreground 13.7 pW 8×10 10 photons/s Hughes et al. 1998 2 arcmin dia. 5 sources > 1mJy (0.05 fW) (300,000 photons/s) CMB 2.7K backlight 0.6 pW 3.6×10 9 photons/s

46. Effective Bolometer Noise Spectral Density 1/f from environment time constant of detector Astronomical signal must be modulated! Atmosphere

47. Chopping vs Rastering Three aspects of mm-wavelength bolometry drive the observational modes: Three aspects of mm-wavelength bolometry drive the observational modes: –High Background – Signal/Background ~ 10 -5 => Raster preferred to Jiggle chop –Atmosphere => Need algorithm to clean (jiggle preferred to raster?) –Detector Time Constant => Limits speed of any continuous motions

48. Advantages to Chopping focus integration time on FOV-sized region low frequency stability not required

49. Advantages to Chopping focus integration time on FOV-sized region low frequency stability not required

50. Disadvantages to Chopping sensitive to differential pickup from dish (secondary support, temperature gradients, etc.) resolve out large scale structure

51. PCA Atmosphere Cleaning Detector Power Spectral Density [nV/rt(Hz)] 10 100 Frequency [Hz] 0.11 10 Raw Signal PCA cleaned (3,2)

52. AzTEC Rastering Gives Uniform Coverage 26 22 17 13 9 4 0 Per-pixel Integration Time [s]

53. AzTEC Rastering Gives Uniform Coverage 26 22 17 13 9 4 0 Per-pixel Integration Time [s]

54. AzTEC Rastering Gives Uniform Coverage 26 22 17 13 9 4 0 Per-pixel Integration Time [s]

55. AzTEC Rastering Gives Uniform Coverage 26 22 17 13 9 4 0 Per-pixel Integration Time [s]

56. AzTEC Rastering Gives Uniform Coverage 26 22 17 13 9 4 0 Per-pixel Integration Time [s]

57. AzTEC Rastering Gives Uniform Coverage 26 22 17 13 9 4 0 Per-pixel Integration Time [s]

58. AzTEC/GOODS-N

59. AzTEC/JCMT05B ‘Local’ Studies Field Size [arcmin 2 ] Obs Time [hrs] target σ [mJ] PI MBM-1217,662 20 (20) 10Williams IC348/Taurus (B.D.) 20 (xN) 32.2 (32.2) 0.8Mohanty UCHII fields 20 (x52) 9.9 (26) 5Kerton Class 0’s in GMCs 20 (x80) 12 (12) 9Hatchel G216, IC443, W3 12.5 deg 2 4.1 (30) 10Moore M83, M51 400 11 (24) 1Wall M311238 13 (24) 3Loinard NGC441420 31 (30) 0.5Braine

60. Raster Observations … OMC1 Johnstone & Bally 1999 SCUBA AzTEC

61. … and Jiggle Mapping Extended emission around ultra-compact HII regions PI: Kerton PRELIMINARY

62. AzTEC image of 4C41.17 HzRG850.2 HzRG850.3 HzRG850.1 4C41.17

64. AzTEC/SHADES - LH 0.5 deg 2 blank field - Lockman Hole BOLOCAM

65. AzTEC/COSMOS Sources Scott et al. (2008) Scott et al. (2008) >3.5 sigma sources identified by circles with diameters equal to twice the AzTEC FWHM on the JCMT; map has been trimmed to “75% coverage region”; average RMS noise level of 1.3 mJy/beam

66. Coverage Map

67. VLA Comparison Plot of the AzTEC 75% coverage region with >3.5 sigma sources circled in black. Purple circles indicate locations of the VLA 1.4 GHz radio sources. 40% (15) of the AzTEC sources have at least one VLA source located within 9 arcsec, and 2 AzTEC sources have 2 VLA counterparts.

68. Stacking Analysis Plot of the stacked AzTEC flux at the VLA source locations for radio sources within the 75% uniform coverage region (452 radio sources; Schinnerer et al. 2007). The signal to noise at the peak is 11. Since 17 radio sources lie close to bright AzTEC sources, so without including 17 radio source positions, and the signal to noise is 8, most of the stacked AzTEC flux is coming from pixels that fall below the source detection threshold (Scott et al. 2008). Plot of the stacked AzTEC flux at the VLA source locations for radio sources within the 75% uniform coverage region (452 radio sources; Schinnerer et al. 2007). The signal to noise at the peak is 11. Since 17 radio sources lie close to bright AzTEC sources, so without including 17 radio source positions, and the signal to noise is 8, most of the stacked AzTEC flux is coming from pixels that fall below the source detection threshold (Scott et al. 2008).

69. Correlation Amplitude A clustering strength between AzTEC and VLA sources is computed using the catalogs. An estimator based on Landy & Szalay (1993) is used. Bias and variance of estimators for W(θ); this means radio and AzTEC sources are clustered at 15’’ and smaller scales, beyond being counterparts to each other. W(θ); this means radio and AzTEC sources are clustered at 15’’ and smaller scales, beyond being counterparts to each other.

70. Postage stamp images of the 22 AzTEC-COSMOS sources are shown below. The six greyscale images represent a 20"x20" box centered on the Subaru i-band, IRAC 3.6 micron, 4.5 micron, 5.8 micron, and 8.0 micron, and MIPS 24 micron images. The AzTEC contours are shown in blue lines over the 8.0 micron image (levels are 4, 5, 6, 7, and 8 mJy). Postage stamp images of the 22 AzTEC-COSMOS sources are shown below. The six greyscale images represent a 20"x20" box centered on the Subaru i-band, IRAC 3.6 micron, 4.5 micron, 5.8 micron, and 8.0 micron, and MIPS 24 micron images. The AzTEC contours are shown in blue lines over the 8.0 micron image (levels are 4, 5, 6, 7, and 8 mJy). AzTEC The VLA 1.4 GHz continuum contours are shown in red superposed over the Subaru i-band image (levels are 30, 40, 60, & 100 micronJy). The VLA 1.4 GHz continuum contours are shown in red superposed over the Subaru i-band image (levels are 30, 40, 60, & 100 micronJy).

73. Continued Study on SMGs Derive most accurate number counts to date. Derive most accurate number counts to date. Quantify cosmic variance. Quantify cosmic variance. Verify/characterize overdensity of SMGs around biased regions. Verify/characterize overdensity of SMGs around biased regions. Determine host halo masses via angular correlation analysis for both biased regions and in the field. Determine host halo masses via angular correlation analysis for both biased regions and in the field. Constrain starburst time scales. Constrain starburst time scales. Constrain stellar initial mass function. Constrain stellar initial mass function.

74. Mo & White (2002) Simulation by Neal Katz

75. Future Study There is still lots to do to characterize AzTEC data: –Known issues in the current analysis pipeline –A few mysteries still to be solved –Better noise estimations –Calculations of false detection rates, biases, and completeness –Fluctuation analysis And a lot to do in terms of source follow-up: –Spitzer proposals are in –VLA observations of FLS field start soon –SMA proposals are in –Gemini proposals are in –HST … next cycle