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Center for Astrophysical Sciences at Johns Hopkins University 1

Center for Astrophysical Sciences at Johns Hopkins University 1. Baltimore, Maryland, USA. Node Coordinator: Tim Heckman Alex Szalay, professor Tamas Budavari, postdoc Charles Hoopes, postdoc. Center for Astrophysical Sciences at Johns Hopkins University. Baltimore, Maryland, USA.

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Center for Astrophysical Sciences at Johns Hopkins University 1

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  1. Center for Astrophysical Sciences at Johns Hopkins University 1 Baltimore, Maryland, USA Node Coordinator: Tim Heckman Alex Szalay, professor Tamas Budavari, postdoc Charles Hoopes, postdoc

  2. Center for Astrophysical Sciences at Johns Hopkins University Baltimore, Maryland, USA • ACS: Advanced Camera for Surveys • JHU/GSFC Co-op • Apache Point Observatory • FUSE: Far Ultraviolet Spectroscopic Explorer • GALEX: Galaxy Evolution Explorer

  3. Center for Astrophysical Sciences at Johns Hopkins University Baltimore, Maryland, USA • ACS: Advanced Camera for Surveys • JHU/GSFC Co-op • Apache Point Observatory • FUSE: Far Ultraviolet Spectroscopic Explorer • GALEX: Galaxy Evolution Explorer

  4. Center for Astrophysical Sciences at Johns Hopkins University Baltimore, Maryland, USA • ACS: Advanced Camera for Surveys • JHU/GSFC Co-op • Apache Point Observatory • FUSE: Far Ultraviolet Spectroscopic Explorer • GALEX: Galaxy Evolution Explorer Cooperative agreement for Research in astrophysics Between JHU and GSFC Laboratory for High Energy Astrophysics (LHEA)

  5. Center for Astrophysical Sciences at Johns Hopkins University Baltimore, Maryland, USA • ACS: Advanced Camera for Surveys • JHU/GSFC Co-op • Apache Point Observatory • FUSE: Far Ultraviolet Spectroscopic Explorer • GALEX: Galaxy Evolution Explorer

  6. Apache Point ObservatoryCloudcroft, New Mexico • SDSS telescopes • ARC 3.5 meter • SPIcam – optical imager • 5’ FOV • 0.14 “/pix • Echelle spectrograph • 3500 to 9800Å • R=37,500 • Double Imaging Spectrograph • Simultaneous red and blue spectra • 3600 to 8000Å – 0.8 to 3 Å/pixel • GrIm II infrared imager and spectrograph • 1μm to 2.5μm • NIC-FPS – NIR camera and Fabry-Perot Spectrometer • 0.85 to 2.5 μm • JHU has a share of the time, and we have experience

  7. Center for Astrophysical Sciences at Johns Hopkins University Baltimore, Maryland, USA • ACS: Advanced Camera for Surveys • JHU/GSFC Co-op • Apache Point Observatory • FUSE: Far Ultraviolet Spectroscopic Explorer • GALEX: Galaxy Evolution Explorer

  8. Far Ultraviolet Spectroscopic Explorer (FUSE) • Spectroscopy from 905 – 1180Å, velocity resolution ~20 km s-1 • Tim Heckman and Charles Hoopes are affiliated with the FUSE Science Team • FUSE Science • Metallicity of neutral gas in I Zw 18 • (Aloisi et al. 2003) • 105 K gas in starburst superwinds • (Heckman et al. 2001, Hoopes et al. 2003) • H2 absorption in starbursts • (Hoopes et al. 2004) • FUV SEDs and Extinction in starbursts • (Buat et al. 2002) • FUV stellar libraries for OB stars • (Pellerin et al. 2002, Robert et al. 2003) Currently in safe mode, but expected to return to service I Zw 18: Aloisi et al. 2003

  9. Center for Astrophysical Sciences at Johns Hopkins University Baltimore, Maryland, USA • ACS: Advanced Camera for Surveys • JHU/GSFC Co-op • Apache Point Observatory • FUSE: Far Ultraviolet Spectroscopic Explorer • GALEX: Galaxy Evolution Explorer

  10. GALEX: The Galaxy Evolution Explorer • Launched April 28, 2003 • Imaging in two UV bands • FUV: λ=1516Å, Δλ=268Å • NUV: λ=2267Å, Δλ=732Å • Spatial resolution ~5” • FOV ~1.2 deg2 • Slitless Spectroscopy • 1350-2800Å • R=80-300 • Tamas Budavari, Alex Szalay, Tim Heckman, Charles Hoopes on the GALEX Science Team

  11. GALEX Surveys * Planned area

  12. Probing Galaxy Evolution with GALEX • Combo-17 • NOAO Deep Wide-Field Survey (NDWFS) • Ultraviolet Luminous Galaxies

  13. COMBO-17 / CDFS • 17 band optical photometry (Wolf et al. 2004) • Photometric redshifts with δz/(1+z)<0.1 at R=24 • Redshifts out z=1 Combo-17 filters

  14. GALEX CDFS Data • GALEX FUV (1500Å) and NUV (2300Å) • Part of the Deep Imaging Survey (DIS) • CFDS_00: 44 ksec, 1sq deg • AB=25 in FUV,NUV • CDFS_01: 31 ksec, 1 sq deg • GALEX data are public as of January 2005

  15. Evolution in the Mass-Dependent Star Formation History of Galaxies from z=0 to 1 • Use GALEX + (aperture corrected) Combo-17 photometry and library of BC03 models (following Kauffmann et al., Salim et al., etc) to derive: • SFR, UV Extinction, Stellar Mass • From GEMS catalog: • Sersic indices, Half-light radii, Surface mass density, SFR/area • Extend work of Kauffmann et al. and Brinchmann et al. to z=1 • Examine SFR distribution vs. many parameters as a function of redshift (Mass, surface density, SFR, extinction, size, Sersic index) • Examine how SFR/M, SFR/size, Extinction varies with mass, surface density

  16. NOAO Deep Wide-Field Survey (NDWFS)co-PIs: Arjun Dey & Buell Jannuzi • Deep optical and NIR survey of two 9.3 sq. deg. fields • Boötes Field (NGPDWS) – North Galactic Pole • Cetus Field – Roughly 30 degrees from SGP • KPNO and CTIO 4-meters, MOSAIC • Survey detection limits (5σ): • BW, R, I – AB=26 • J,H,K – AB = ~21 • Survey Status • All data obtained • Boötes field public release in October 2004: BWRIK images, single-band and matched catalogs

  17. GALEX Observations of Bootes • GALEX Coverage of Boötes field • DIS (AB = 25 in NUV, FUV) 9 sq. deg. (not yet complete) • UDIS (AB = 26 in NUV, FUV) 1 sq. deg. (soon will have 90,000 seconds!) • DSS (AB = 22.5-24) 1 sq. deg. • Additional U-band data in Boötes field (GALEX/NDWFS collaboration) • Entire field imaged to AB=25 • 1 sq. deg. imaged to AB=26 • Observations planned or taken with Chandra, Spitzer, VLA FIRST, Redshifts from MMT Hectospec (AGES), Gemini GMOS

  18. Steidel et al. 2003

  19. GALEX-NDWFS 2 color diagram

  20. GALEX-NDWFS 2 color diagram

  21. GALEX-NDWFS Science Star Formation and Extinction Properties of Galaxies at z=1 and 2 • Once high-z populations are isolated, derive LF, extinction corrections, corrected LF, SFR density to compare with z≥3 • Need better redshifts than dropout technique • Spitzer IRAC data to improve SEDs for photo-z, and MIPS data to compare UV/FIR • Use Lyman break in DSS to isolate z~0.6 sample Investigation of Galaxies at Intermediate Redshifts in the AGES sample • Redshifts and multiwavelength data for galaxies with I<20 • NIR + Optical + UV spectral evolution modeling, following to Salim et al. (2004)

  22. Ultraviolet Luminous Galaxies (UVLGs) • First sample described in Heckman et al. (2005) • Matched GALEX All-Sky Imaging Survey IR0.2 with SDSS DR1 galaxies (Seibert et al. 2005) • 74 “UV luminous” galaxies (LFUV>2×1010 L๏)between 0.1<z<0.3 [L* = 4×109L๏ at z=0 (Wyder et al. 2005), L* = 6×1010L๏ at z=3 (Arnouts et al. 2005)] • Co-moving density 10-5 Mpc-3 (>100× less than LBGs at z=3) • Additional properties (metallicities, age indicators, SFRs, stellar mass, etc.) • SDSS value-added catalogs (www.mpa-garching.mpg.de/SDSS)* • Spectral evolution modeling by Salim et al. (2005) • Recently increased sample to 204 using DR2 and IR0.9 *see Kauffmann et al. 2004, Brinchmann et al. 2004, Tremonti et al. 2004

  23. Structural Properties FUV Luminosity vs. Half-light Radius • UVLGs span a large range in size • No correlation between LFUV and size • Strong correlation between IFUV and stellar mass • “Large” UVLGs (IFUV<108 L๏ kpc-2) • Massive (log M*=10.5 – 11.3) • High-mass disk systems with young stellar population • “Compact” UVLGs (IFUV>108 L๏ kpc-2) • Low mass (log M*=9.5 – 10.7) • Mass range similar to LBGs (L๏/kpc2) (kpc) (L๏)

  24. Structural Properties FUV Surface Brightness vs. Stellar Mass • UVLGs span a large range in size • No correlation between LFUV and size • Strong correlation between IFUV and stellar mass • “Large” UVLGs (IFUV<108 L๏ kpc-2) • Massive (log M*=10.5 – 11.3) • High-mass disk systems with young stellar population • “Compact” UVLGs (IFUV>108 L๏ kpc-2) • Low mass (log M*=9.5 – 10.7) • Mass range similar to LBGs (L๏ kpc-2) Compact Large (M๏)

  25. Compact UVLGs

  26. Large UVLG: SDSS J010126.56+133245.5 FUV NUV

  27. Compact UVLG: SDSS J005527.45-002148.6 FUV NUV

  28. Population Comparison (slide courtesy C. Martin)Large UVLGs, Compact UVLGS, LBGs M* Log LUV Log rUV AUV Log b [O/H] 12 1.5 12 3 2 9 11 1 11 2 1 8.5 10 0.5 10 1 0 8 9 9 9 0 -1 7.5

  29. What’s next for UVLGs? (Multiwavelength Analysis of UVLGPOPulation!) • Larger sample from SDSS DR3 and GR1 • ACS/NICMOS imaging of a subsample • Morphologies • Presence of older stars • Spitzer FIR • Chandra

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