osiris spectroscopy of supercompact uv luminous galaxies

© 2003 By Default!

A Free sample background from www.powerpointbackgrounds.com

Slide 1

Thiago S. GonçalvesCaltech

© 2003 By Default!


Slide 2

CaltechCaltechThiago S. GonçalvesThiago S. Gonçalves

Chris MartinChris Martin

Ted WyderTed Wyder

Antara Basu-ZychAntara Basu-Zych

David SchiminovichDavid Schiminovich

Matt O’DowdMatt O’Dowd

Tim HeckmanTim Heckman

Roderik OverzierRoderik Overzier

ColumbiaColumbia

MPA, GarchingMPA, Garching

JHUJHU

© 2003 By Default!


Slide 3

UVLGs: general characteristicsUVLGs: general characteristics

• Heckman et al (2005), Hoopes et al. Heckman et al (2005), Hoopes et al. (2007)(2007)

• Detected by GALEX in the FUV withDetected by GALEX in the FUV withLLFUVFUV ≥ 2×10 ≥ 2×101010 L L, , II15301530 ≥ 10 ≥ 1099 L L kpc kpc-2-2

• Low dust attenuation, young populations Low dust attenuation, young populations (Basu-Zych et al. 2007)(Basu-Zych et al. 2007)

• Similar morphological indices to high- Similar morphological indices to high- redshift LBGsredshift LBGs

© 2003 By Default!


Slide 4

Overzier et alOverzier et al

© 2003 By Default!


Slide 5

UVLG0926

S/N map

• 2hr exposures

• Pa-α emission line

© 2003 By Default!


Slide 6

σ mapVelocity map

© 2003 By Default!


Slide 8

σ's similar to LBGs (Law et al. 2007)σ's similar to LBGs (Law et al. 2007)σ map

Velocity map

© 2003 By Default!


Slide 10

SummarySummary

• Complementary data to understand Complementary data to understand

UVLG dynamics: HST optical and IFUUVLG dynamics: HST optical and IFU

• Opportunity to study Lyman Break Opportunity to study Lyman Break

analogs at higher S/N ratios and analogs at higher S/N ratios and

spatial resolutionspatial resolution

• 4 more nights coming - so stay 4 more nights coming - so stay

tuned!tuned!

osiris spectroscopy of supercompact uv luminous galaxies

Documents