Center for Astrophysical Sciences at Johns Hopkins University 1

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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

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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

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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

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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)
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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

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Apache Point ObservatoryCloudcroft, New Mexico

• SDSS telescopes
• ARC 3.5 meter
• SPIcam optical imager
• 5 FOV
• 0.14 /pix
• Echelle spectrograph
• 3500 to 9800Å
• R37,500
• 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

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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

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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
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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

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GALEX The Galaxy Evolution Explorer

• Launched April 28, 2003
• Imaging in two UV bands
• FUV ?1516Å, ??268Å
• NUV ?2267Å, ??732Å
• Spatial resolution 5
• FOV 1.2 deg2
• Slitless Spectroscopy
• 1350-2800Å
• R80-300
• Tamas Budavari, Alex Szalay,
  Tim Heckman, Charles
  Hoopes on the GALEX Science
  Team

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GALEX Surveys
Name Area (Sq. deg.) Exposure (seconds) Mlim galaxies ltzgt
All-sky Imaging Survey (AIS) 35,000 100 20.5 107 0.2
Medium Imaging Survey (MIS) 1,000 1,500 23 106.5 0.6
Deep Imaging Survey (DIS) 80 30,000 25 107 0.8
Ultradeep Imaging Survey (UIS) 4 200,000 26 105.5 0.9
Nearby Galaxy Survey (NGS) 200 1,500 27 arcsec-2 200 0.001
Wide-field Spec. Survey (WSS) 80 30,000 20 104.5 0.15
Medium Spec. Survey (MSS) 8 300,000 21-23 104.5 0.5
Deep Spec. Survey (DSS) 2 1,500,000 22.5-24 104.5 0.9
Planned area
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Probing Galaxy Evolution with GALEX

• Combo-17
• NOAO Deep Wide-Field Survey (NDWFS)
• Ultraviolet Luminous Galaxies

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COMBO-17 / CDFS

• 17 band optical photometry (Wolf et al. 2004)
• Photometric redshifts with dz/(1z)lt0.1 at R24
• Redshifts out z1

Combo-17 filters
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GALEX CDFS Data

• GALEX FUV (1500Å) and NUV (2300Å)
• Part of the Deep Imaging Survey (DIS)
• CFDS_00 44 ksec, 1sq deg
• AB25 in FUV,NUV
• CDFS_01 31 ksec, 1 sq deg
• GALEX data are public as of January 2005

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Evolution in the Mass-Dependent Star Formation
History of Galaxies from z0 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 z1
• 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

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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 (5s)
• BW, R, I AB26
• J,H,K AB 21
• Survey Status
• All data obtained
• Boötes field public release in October 2004
  BWRIK images, single-band and matched catalogs

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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 AB25
• 1 sq. deg. imaged to AB26
• Observations planned or taken with Chandra,
  Spitzer, VLA FIRST, Redshifts from MMT Hectospec
  (AGES), Gemini GMOS

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Steidel et al. 2003
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GALEX-NDWFS 2 color diagram
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GALEX-NDWFS 2 color diagram
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GALEX-NDWFS Science

• Star Formation and Extinction Properties of
  Galaxies at z1 and 2
• Once high-z populations are isolated, derive LF,
  extinction corrections, corrected LF, SFR density
  to compare with z3
• 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 z0.6 sample
• Investigation of Galaxies at Intermediate
  Redshifts in the AGES sample
• Redshifts and multiwavelength data for galaxies
  with Ilt20
• NIR Optical UV spectral evolution modeling,
  following to Salim et al. (2004)

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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 (LFUVgt21010 L?)
  between 0.1ltzlt0.3
• L 4109 L? at z0 (Wyder et al. 2005), L
  61010 L? at z3 (Arnouts et al. 2005)
• Co-moving density 10-5 Mpc-3 (gt100 less than
  LBGs at z3)
• Additional properties (metallicities, age
  indicators, SFRs, stellar mass, etc.)
• SDSS value-added catalogs (www.mpa-garching.mpg.d
  e/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

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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 (IFUVlt108 L? kpc-2)
• Massive (log M10.5 11.3)
• High-mass disk systems with young stellar
  population
• Compact UVLGs (IFUVgt108 L? kpc-2)
• Low mass (log M9.5 10.7)
• Mass range similar to LBGs

(L?/kpc2)
(kpc)
(L?)
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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 (IFUVlt108 L? kpc-2)
• Massive (log M10.5 11.3)
• High-mass disk systems with young stellar
  population
• Compact UVLGs (IFUVgt108 L? kpc-2)
• Low mass (log M9.5 10.7)
• Mass range similar to LBGs

(L? kpc-2)
Compact
Large
(M?)
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Compact UVLGs
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Large UVLG SDSS J010126.56133245.5
FUV
NUV
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Compact UVLG SDSS J005527.45-002148.6
FUV
NUV
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Population Comparison (slide courtesy C.
Martin)Large UVLGs, Compact UVLGS, LBGs
M
Log LUV
Log rUV
AUV
Log b
O/H
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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
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Whats next for UVLGs?
(Multiwavelength Analysis of UVLG POPulation!)

• Larger sample from SDSS DR3 and GR1
• ACS/NICMOS imaging of a subsample
• Morphologies
• Presence of older stars
• Spitzer FIR
• Chandra