MaDCoWS: The Massive Distant Clusters of WISE Survey -- Sesto Clusters 2013

Talk about MaDCoWS from Sesto Clusters 2013: "Tracing Cosmic Evolution with Clusters of Galaxies"

Transcript

1. MaDCoWS MaDCoWS: The Massive Distant Clusters of WISE Survey Daniel Gettings (University of Florida) Sesto Clusters 2013 02 July 2013 On Behalf of the MaDCoWS Collaboration 1
2. MaDCoWS in Brief Aim: Construct an all-sky sample of IR-selected, massive, z≳1 galaxy clusters Method: Combining WISE and optical data to search for overdensities of z≳1 galaxies Why WISE? WISE combines the powerful 3-5 µm wavelength regime with all-sky coverage Status: Ongoing program of Spitzer, CARMA, and spectroscopic followup with a subsample of 200 candidates in the SDSS DR8 region, in order to: (1) characterize our selection function, and (2) learn how to improve our techniques Significance: A large sample to enable cluster cosmology, galaxy evolution, etc. The last such sample until, and very complementary to, eRosita. MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 2
3. Galaxy Clusters and Cosmology http://www.mpa-garching.mpg.de/galform/millennium/ z=0 z=1.4 z=5.7 z=18.3 NASA/WMAP Science Team z≈1100 http://www.astro.ucla.edu/~wright/cosmo_04.htm tUni<~10-32 s SDSS/M. Blanton Williamson+ 2011 MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 3
4. Galaxy Clusters and Cosmology http://www.mpa-garching.mpg.de/galform/millennium/ z=0 z=1.4 z=5.7 z=18.3 NASA/WMAP Science Team z≈1100 http://www.astro.ucla.edu/~wright/cosmo_04.htm tUni<~10-32 s SDSS/M. Blanton Williamson+ 2011 Primordial Non-Gaussianity Physics of Inflation Cosmological Parameters Baryonic Physics Galaxy Evolution Halo Occupation X-Ray vs. SZ vs. Galaxies MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 4
5. Galaxy Evolution in the Densest Environments Tran+ Star-Forming Galaxy Fraction Mancone+ 2010 Other Applications Gonzalez+ 2012b MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 5
6. The WISE Mission Wright+ (2010) ʴ1 Orbit ʴ20 Days One Orbit All-Sky Release: 14 March 2012 irsa.ipac.caltech.edu Data Available from IRSA: Effective Exposure Depth ʙ 1 Full Sky Coverage AllWISE Coming Late 2013: ʙ 2 Full Sky Coverages µm µm λ Coverage Scanning Pattern MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 6
7. How WISE Sees Galaxy Clusters (Vega) Gettings+ 2012 Muzzin+ 2013 MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 7
8. What z>~1 Clusters Look Like in WISE Anthony H. Gonzalez 5 FIG. 2.— SPT-CL J0546-5345, a 1 ×1015M SZ-selected cluster at z = 1.07 (Brodwin et al. 2010). The left panel shows an optical-IRAC color image of the cluster, the middle panel is an IRAC 3.6µm image, and the right panel is the WISE W1 image. overdensities of super-L∗ galaxies in the most massive clusters out to z ∼ 1.5 (and perhaps be- yond) with WISE. Our team has undertaken the groundwork necessary to demonstrate the viability and efficiency of a WISE-based cluster search, including algorithm development, identification of known clusters, identification of limiting systematics, and initial follow-up. Cluster Detection. We carried out an initial test to verify that cluster detection is feasible with the WISE data by inspecting the WISE images for known massive clusters at z > 1. In Figures 2 and 3 we show the WISE and Spitzer/IRAC photometry for two z > 1 clusters from the SPT survey, which are among the most massive known at this epoch. While the WISE resolution (∼ 6 ) results in many blended detections, the clusters remain clearly identifiable in the WISE data. Encouraged, we next consider the best method for cluster detection. Members of our team have experience with a number of different infrared-based cluster detection techniques gained from past programs (e.g. Elston et al. 2006; Eisenhardt et al. 2008; Papovich 2008); for this program we choose to use a color-selection technique. Papovich (2008); Papovich et al. (2010) first demon- strated the power of this approach in the mid-IR, using Spitzer/IRAC data to identify 103 distant cluster candidates in the 50 deg2 SWIRE fields, including a spectroscopically confirmed cluster at z = 1.62. For WISE we have undertaken initial development of a modified version of this de- tection algorithm optimized for the WISE bands. Starting with the WISE catalog, we first restrict Anthony H. Gonzalez 5 FIG. 2.— SPT-CL J0546-5345, a 1 ×1015M SZ-selected cluster at z = 1.07 (Brodwin et al. 2010). The left panel shows an optical-IRAC color image of the cluster, the middle panel is an IRAC 3.6µm image, and the right panel is the WISE W1 image. overdensities of super-L∗ galaxies in the most massive clusters out to z ∼ 1.5 (and perhaps be- yond) with WISE. Our team has undertaken the groundwork necessary to demonstrate the viability and efficiency of a WISE-based cluster search, including algorithm development, identification of known clusters, identification of limiting systematics, and initial follow-up. Cluster Detection. We carried out an initial test to verify that cluster detection is feasible with the WISE data by inspecting the WISE images for known massive clusters at z > 1. In Figures 2 and 3 we show the WISE and Spitzer/IRAC photometry for two z > 1 clusters from the SPT survey, which are among the most massive known at this epoch. While the WISE resolution (∼ 6 ) results in many blended detections, the clusters remain clearly identifiable in the WISE data. Encouraged, we next consider the best method for cluster detection. Members of our team have experience with a number of different infrared-based cluster detection techniques gained from past programs (e.g. Elston et al. 2006; Eisenhardt et al. 2008; Papovich 2008); for this program we choose to use a color-selection technique. Papovich (2008); Papovich et al. (2010) first demon- strated the power of this approach in the mid-IR, using Spitzer/IRAC data to identify 103 distant cluster candidates in the 50 deg2 SWIRE fields, including a spectroscopically confirmed cluster at z = 1.62. For WISE we have undertaken initial development of a modified version of this de- tection algorithm optimized for the WISE bands. Starting with the WISE catalog, we first restrict IRAC W2 SPT-CL J0546-5345 (z=1.06; Brodwin+ 2011) SPT-CL J0205-5829 (z=1.322; Stalder+ 2012) XDCP J0044.0-2033 (z=1.579; Santos+ 2011a) MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 8
9. How to Find Clusters with WISE WISE ASR Source Catalog 563,921,584 sources SDSS-DR8 Photometric Catalog 469,048,604 sources Resulting Overlap Area: ~10,000 deg2 1,899,771,574 sources SuperCOSMOS Sky Survey Northern Option Southern Option First Step: Match with optical data MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 9
10. W1 ‒ 10’ W2 ‒ 10’ W1 ‒ 5’ SDSS i ‒ 5’ Density Map ‒ 20’ SDSS i ‒ 10’ How to Find Clusters with WISE MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 10
11. Wavelet-Smoothed Density Map 12°⁇12° (1º edge overlap) 3°⁇3° How to Find Clusters with WISE MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 11
12. Binning Noise Normal Binning “Drizzle” Binning 10% Scatter 1% Scatter 10% Scatter 1% Scatter Overdensity Significance Overdensity Significance Scatter Scatter MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 12
13. Tuning Search Parameters with SPT and ACT Clusters ( z=1.13, M500=8.39x1014) SPT-CL J2106-5844 (Foley+ 2011) Optical Rejection Spatial Filtering Scale WISE Color Rejection WISE Flux & SNR Cuts WISE Flux & SNR Cuts WISE Color Rejection Spatial Filtering Scale Relative Rank in ~100 deg2 1 2 3 4 5 MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 13
14. First Discovery Paper: MOO J2342.0+1301 W K MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 14
15. Spitzer/IRAC Followup Campaign ✦ Targeting top 200 MaDCoWS cluster candidates ✦ Focusing on SDSS Region ✦ Purpose: Better understanding of Cluster Mass, Cluster Redshift selection functions [3.6] W1 SPT Clusters MaDCoWS Candidates [3.6] – [4.5] (Vega) [4.5] (Vega) NGal( R<1’ ) N SpUDS Fields MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 15
16. Spectroscopic Followup SZ Followup with CARMA Last Semester: First SZ Detection ✦ One new preliminary detection ✦ Many more targets still to be observed This Semester: Current count: 12 clusters at 0.8 < z < 1.2 spectroscopically confirmed (S.A. Stanford et al., in prep) Several nights of Keck/DEIMOS time Ongoing 2nd semester of Gemini-N/GMOS followup MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 16
17. Looking Towards the Future AllWISE 5σ Limits Extending to the South MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 17
18. Summary Aim: Construct an all-sky sample of IR-selected, massive, z≳1 galaxy clusters Method: Combining WISE and optical data to search for overdensities of z≳1 galaxies Why WISE? WISE combines the powerful 3-5 µm wavelength regime with all-sky coverage Status: We are succeeding at using WISE to detect z~1 clusters over large areas. Much more to come! Significance: A large sample to enable cluster cosmology, galaxy evolution, etc. The last such sample until, and very complementary to, eRosita. MaDCoWS MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 18
19. Summary Aim: Construct an all-sky sample of IR-selected, massive, z≳1 galaxy clusters Method: Combining WISE and optical data to search for overdensities of z≳1 galaxies Why WISE? WISE combines the powerful 3-5 µm wavelength regime with all-sky coverage Status: We are succeeding at using WISE to detect z~1 clusters over large areas. Much more to come! Significance: A large sample to enable cluster cosmology, galaxy evolution, etc. The last such sample until, and very complementary to, eRosita. MaDCoWS Thanks! MaDCoWS ʙ Daniel Gettings ʙ Sesto Clusters 2013 19