1. First Results from the WIRED Survey John H. Debes (ORAU/GSFC)

2. Wide-field Infrared Survey Explorer WISE Mission Overview Salient Features 4 imaging channels covering 3 - 25 microns wavelength4 imaging channels covering 3 - 25 microns wavelength 40 cm telescope operating at <17K40 cm telescope operating at <17K Two stage solid hydrogen cryostatTwo stage solid hydrogen cryostat Delta launch from WTR on December 14, 2009Delta launch from WTR on December 14, 2009 Sun-synchronous 6am/6pm 500km orbitSun-synchronous 6am/6pm 500km orbit Scan mirror provides efficient mappingScan mirror provides efficient mapping Operational life: estimate 11 monthsOperational life: estimate 11 months 4 TDRSS tracks per day4 TDRSS tracks per day Science Sensitive all sky survey with 8X redundancySensitive all sky survey with 8X redundancy –Find the most luminous galaxies in the universe –Find the closest stars to the sun –Provide an important catalog for JWST –Provide lasting research legacy National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology

3. What is WIRED? WISE IR Excess around Degenerates (WIRED) Survey Merge WISE catalogue with Sloan, 2MASS, and UKIDSS photometry to discover IR-excess sources around white dwarfs WIRED has the potential to: Detect Dusty White Dwarfs to ~140 pc Detect T2 or earlier companions to 70 pc

4. Sensitivity to Companions Companion sensitivity depends on T eff Taking T eff =10,000 K, WIRED will be sensitive to T2 dwarfs to ~70pc in WISE 1 and WISE 2 bands WD WD+T2

5. Sensitivity to Dust Disks Fiducial Disk: G29-38 WISE S/N=5 sensitivities: 0.08 mJy (3.35μm), 0.1 mJy (4.6μm), 0.8 mJy (12μm) 6 mJy (22μm) Detect IR excess in bands 1 & 2 to ~140 pc Detect strong silicate features out to ~55 pc

6. Selection Criteria Select all Sloan DR4 WDs, search for NIR/WISE band excesses Fit derived parameters to photometry with cooling models to derive provisional distance (Bergeron et al. 1995) Fit significant excesses with companion or disk comparisons See poster by D. W. Hoard for statistics of the survey

7. S/N > 5 >3σ Selection Criteria Model WD photosphere Companion doesn’t fit=disk candidate

8. Sanity Checks

10. Previously Reported Dusty White Dwarfs GD 40 WISE1=0.26+/-0.02 mJy WISE2=0.20+/-0.02 mJy IRAC1=0.23+/-0.01 IRAC2=0.19+/-0.01

11. Previously Reported Dusty White Dwarfs WD 1150-153 WD Photosphere Model Disk Model R in =13 R ∗

12. New Candidates WIRED 1--WD+Disk T eff =6880 K D=86 pc

13. New Candidates WIRED 2--WD+Disk T eff =8900 K

14. New Candidates WIRED 3--WD+L5 T eff =8100 K

15. Conclusions The tip of the iceberg--many more interesting sources to be found! WIRED will provide variability info for known dusty white dwarfs WISE will provide legacy information as known WDs become complete to ~100pc (currently, only complete to ~20pc) In May 2011, preliminary WISE catalogue will be publicly available In April 2012 full catalogue will be available

16. The WIRED Team Stefanie Wachter, (IPAC, lead) Don W. Hoard (IPAC) Dave T. Leisawitz (GSFC) Martin Cohen (UCLA)

17. WISE Science Team Dominic Benford - GSFC Andrew Blain - Caltech Martin Cohen - UCB Roc Cutri - IPAC Peter Eisenhardt -JPL Nick Gautier - JPL Tom Jarrett - IPAC Davy Kirkpatrick - IPAC David Leisawitz - GSFC Carol Lonsdale - NRAO Amy Mainzer - JPL John Mather - GSFC Ian McLean - UCLA Robert McMillan - UA Bryan Mendez - UCB Deborah Padgett - IPAC Michael Ressler - JPL Michael Skrutskie - UVa Adam Stanford - LLNL Russell Walker - MIRA PI: Edward L. Wright - UCLA National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology