Duilia de Mello (CUA-GSFC) Amy Soto (CUA), Nick Bond (GSFC), Jon P. Gardner (GSFC), Swara...
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Transcript of Duilia de Mello (CUA-GSFC) Amy Soto (CUA), Nick Bond (GSFC), Jon P. Gardner (GSFC), Swara...
Duilia de Mello (CUA-GSFC)
Amy Soto (CUA), Nick Bond (GSFC), Jon P. Gardner (GSFC), Swara Ravindranath (STScI), Claudia Scarlata (UMN), Elysse
Voyer (LAM), Harry Teplitz (IRSA)
Elmegreen et al. 05UDF i image (lines=0.5”)
884 gals with d >0.3”114 chain178 clump cluster126 double97 tadpole269 spiral100 elliptical
Clump cluster propertieszphot= 1.6 - 36x108 Msun
D = 1.8 kpc5 – 10 clumps per galaxy
Simulations: high-z clumps could both dissipate to form Simulations: high-z clumps could both dissipate to form
disks and coalesce to form bulges (e.g., Bournaud et al disks and coalesce to form bulges (e.g., Bournaud et al
2011; Ceverino et al. 2010, Krumholz et al. 2010; Agertz et 2011; Ceverino et al. 2010, Krumholz et al. 2010; Agertz et
al. 2009; Elmegreen 2008) – potential building block of local al. 2009; Elmegreen 2008) – potential building block of local
spiralsspirals
Simulation
Ceverino et al. 10
Bournaud et al. 11
(Faucher-Giguere's
Perret's
simulations)
When UV Clumps become disks?
z < 1.5 – restframe UV
Instruments:
WFPC2 F300W U band (de Mello et al. 2006, Voyer et al. 2009)
ACS SBC F150LP (Voyer et al. 2011)
BUT more recently WFC3 UVIS (de Mello, Soto, Bond, Teplitz)
Voyer et al. (2011, 2013)
230 FUV selected galaxies (0.1<z<1.2) ACS/SBC F150LP GOODS-N and S
104.5 Lsun < LFUV < 108 Lsun
Optical morphologies (GALFIT) compared to spectral types (SED fitting)
Majority of unobscured star formation occurs in:
Spectral type typical of quiescent disks almost evenly in Sersic (n) typical of disks and clumpy merger/tidal morphologies
~50% of Starburst STs have disky morphologies
disky
n<0.8 mergers
0.8<n<2.5 disks
n>2.5 Early-type
Ravindranath+Lotz+
uvu
df.i
pac
.ca
ltec.
ed
u
Teplitz et al. 2013 arXiv 0711360
Charge Transfer Efficiency CTEarrows = readout direction
CTE degradationEffect is worse for objects far fromCCD readout(Solar activity)
Epoch 3 – post-flash (unbinned)
ACS WFC3F275W
WFPC2 F300W
phot-z 0.63
0.57
0.77
1.18
270 objects
ACS WFC3F275W
WFPC2 F300W
phot-z 0.63
0.57
0.77
1.18
270 objects
Templates: early- to late-type Coleman et al.Starbursts Kinney et al.
E Sbc Scd
Im Starburst Starburst
2 spheroids3 chains4 clump clusters5 irregulars6 spirals7 clumpy disks
rest-frame 3000 A 1500 A color (1500-3000) 7000A
Bond et al. 2013
Bond et al. 2013
rest-frame 3000 A 1500 A color (1500-3000) 7000A
ID5: (4”x4”)
Redshift: 0.57
WFPC2 F300W – Voyer et al. (2013) WFC3 F275W
ID5 with contour levels 6 – 11σ
Redshift: 0
ID5-Clump Area Comparison
1
2
3
4
5
6Clump 2 Clump
3
Clump 4
Clump 6
Contours are ≥ 6 σClump 5 is 4σ
Sizes:0.8 to 1.6 kpc
ID17: (2.5”x2.5”)
ID17: (2.5”x2.5”) with contour level 5σ
Redshift: 1.18
WFC3 F275WWFPC2 F300W
zoomed in clumps
Redshift: 1.18
Sizes1.6 kpc1.3 kpc0.7 kpc0.8 kpc
F275Wz ~ 0.8 = rest frame 1500 AA
Sta
rbur
st99
1000 – 2500A
Why UV?
Giant HII regions/Super OB associations
Powered by massive young clusters with 100 to 1000 O/WR stars, instead of a few as in regular HII regions (Zinnecker & Yorke ARAA 2007).
The Carina Nebula in the Milky Way – 150 pc
30 Doradus in the LMC – 100 pc (radius)
NGC 604 in M33 – 200 pc (radius)
200 pc radius
Giant Spiral: NGC6872
D=65 Mpc size > 100 Kpc Eufrasio et al. (2013)
NGC 3079
Petty et al. 2009
GALEX UV images redshifted to z ~ 1.5 and z ~4resembles LBGs (Gini, M20, Sersic)
Careful when using UV to study overall properties of galaxies
There are UV clumps without clear signatures of disks
Most of UV clumps seem to be in disks at z ~ 1
UV clumps are much larger than HII regions, SSCs, etc
Found no signatures of size evolution in UV clumps at z~1 in comparison with higher-z