resolved stellar populations outside the local group alessandra aloisi (stsci/esa) science with the...
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Resolved Stellar Populations outside the Local Group
Alessandra Aloisi (STScI/ESA)
Science with the New HST after SM4Bologna – 30 January 2008
Collaborators
F. Annibali, A. Grocholski, C. Leitherer, J. Mack, M. Sirianni, & R. van der Marel (STScI)
L. Angeretti, G. Clementini, R. Contreras, G. Fiorentino, M. Maio, D. Romano, & M. Tosi (INAF-OAB)
M. Marconi & I. Musella (INAF-OAC)E. Held & L. Greggio (INAF-OAP)
A. Saha (NOAO)
Hierarchical Galaxy Formation
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• dwarf galaxies first to form stars
• bigger galaxies form by merging of these building blocks
High-mass galaxies’ oldest pop must be as old as low-mass galaxies’ pop or younger
Mapping Galaxy Formation
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Mapping Galaxy Formation
1. High-Redshift Studies looking directly back in time by observing distant galaxies (e.g. HDFs, GOODS, HUDF)
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Mapping Galaxy Formation
1. High-Redshift Studies looking directly back in time by observing distant galaxies (e.g. HDFs, GOODS, HUDF)
Mapping Galaxy Formation
1. High-Redshift Studies looking directly back in time by observing distant galaxies (e.g. HDFs, GOODS, HUDF)
2. Stellar Archaeology studying nearby galaxies by resolving their present-day stellar populations
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Mapping Galaxy Formation
1. High-Redshift Studies looking directly back in time by observing distant galaxies (e.g. HDFs, GOODS, HUDF)
2. Stellar Archaeology studying nearby galaxies by resolving their present-day stellar populations
2
Mapping Galaxy Formation
1. High-Redshift Studies looking directly back in time by observing distant galaxies (e.g. HDFs, GOODS, HUDF)
2. Stellar Archaeology studying nearby galaxies by resolving their present-day stellar populations
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Courtesy Elena Sabbi (STScI)
Resolving Galaxies with HST Imaging
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Resolving Galaxies with HST Imaging
• images in multiple bands BVI (optical) & JH (NIR)
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Resolving Galaxies with HST Imaging
Sextans ACTIO• images in multiple bands
BVI (optical) & JH (NIR)
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Hunter (1997)
Resolving Galaxies with HST Imaging
Sextans ACTIO
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Hunter (1997)
Sextans AHST/WFPC2
Dohm-Palmer et al. (2002)
• images in multiple bands BVI (optical) & JH (NIR)
Resolving Galaxies with HST Imaging
Sextans A
Dolphin et al. (2003)
Sextans A
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• images in multiple bands BVI (optical) & JH (NIR)
• CMD of resolved stars
Resolving Galaxies with HST Imaging
Dolphin et al. (2003)
Sextans A
RGBT
TP-AGB (C stars)
Cepheids• images in multiple bands BVI (optical) & JH (NIR)
• CMD of resolved stars
• distance RGBT, TP-AGB, Cepheids
3
Resolving Galaxies with HST Imaging
Sextans A
RGBT
TP-AGB (C stars)
Cepheids• images in multiple bands BVI (optical) & JH (NIR)
• CMD of resolved stars
• distance RGBT, TP-AGB, Cepheids
• star formation history
Aparicio & Gallart (2004)
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TO
Resolving Galaxies with HST Imaging
Sextans A
RGBT
TP-AGB (C stars)
Cepheids• images in multiple bands BVI (optical) & JH (NIR)
• CMD of resolved stars
• distance RGBT, TP-AGB, Cepheids
• star formation history
Aparicio & Gallart (2004)
3
TO
All galaxies studied in sufficient detail so far contain ancient populations
What does it really mean to go outside the Local Group?
Grebel (1999)
• distance > 1 Mpc
• different types of galaxies accessible:
Giant Ellipticals
Active Galaxies (starbursts & BCDs)
• only filters F606W & F814W really feasible !
dSphsdEsdSph/dIrrsdIrrs
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What is beyond the Local Group?
Courtesy Tom Brown (STScI)
closest giant EllipticalNGC 5128 (Centaurus group)
D = 3.8 Mpc
closest Starburst NGC 1569 (IC 342 group ? )
D = 3.2 Mpc
closest metal-poor BCDUGC 4483 (M81 group)
D = 3.4 Mpc
and more …
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The Closest Giant Elliptical: NGC 5128
NGC 5128 WEH
• some fields (r < 30 kpc) observed with WFPC2 down to the RGBT
• deepest field (r ~ 37 kpc) observed with ACS/WFC down to the RC
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The Closest Giant Elliptical: NGC 5128
NGC 5128 WEH
• some fields (r < 30 kpc) observed with WFPC2 down to the RGBT
• deepest field (r ~ 37 kpc) observed with ACS/WFC down to the RC
6Rejkuba et al. 2005
The Closest Giant Elliptical: NGC 5128
NGC 5128 WEH
• some fields (r < 30 kpc) observed with WFPC2 down to the RGBT
• deepest field (r ~ 37 kpc) observed with ACS/WFC down to the RC
6Rejkuba et al. 2005
Metal-rich all the way out !
Mean [M/H] = – 0.64
Mean Age = 8.5 Gyrs
Similarities with M31 Halo in the LG
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M31
Similarities with M31 Halo in the LG
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M31 haloACS/WFC
Brown et al. (2003)
Similarities with M31 Halo in the LG
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M31 haloACS/WFC
Brown et al. (2003)
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
The Closest Starburst: NGC 1569
• deep field observed with ACS/WFC down to the RC
• distance is 1 Mpc larger than previously
believed D = 3.2 Mpc
• RC/HB at the detection limit
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NGC 1569ACS/WFC
The Closest Starburst: NGC 1569
• deep field observed with ACS/WFC down to the RC
• distance is 1 Mpc larger than previously
believed D = 3.2 Mpc
• RC/HB at the detection limit
Grocholski, Aloisi et al. (in prep.)
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NGC 1569ACS/WFC
V – I
I
Grocholski, Aloisi et al. (in prep.)
The Closest Starburst: NGC 1569
• deep field observed with ACS/WFC down to the RC
• distance is 1 Mpc larger than previously
believed D = 3.2 Mpc
• RC/HB at the detection limit
Grocholski, Aloisi et al. (in prep.)
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NGC 1569ACS/WFC
V – I
I
Grocholski, Aloisi et al. (in prep.)Grocholski, Aloisi et al. (in prep.)
I
V – I
[Fe/H] = – 1.0 NGC 1569 Halo1Gyr 3Gyr 10Gyr
The Closest Starburst: NGC 1569
• deep field observed with ACS/WFC down to the RC
• distance is 1 Mpc larger than previously
believed D = 3.2 Mpc
• RC/HB at the detection limit
Morphology of RGB, presence of RC and lack (?) of HB suggest metal-rich and intermediate-age stars in the halo once again !
Grocholski, Aloisi et al. (in prep.)
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NGC 1569ACS/WFC
V – I
I
Grocholski, Aloisi et al. (in prep.)Grocholski, Aloisi et al. (in prep.)
I
V – I
[Fe/H] = – 1.0 NGC 1569 Halo1Gyr 3Gyr 10Gyr
The Closest Metal-Poor BCD: UGC 4483• deep field observed with WFPC2 down to the RGB
Izotov & Thuan (2002)
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UGC 4483ACS/WFC
I
V – I
The Most Metal-Poor BCD at the borders of the Local Volume: I Zw 18
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RGB Stars in I Zw 18
11Aloisi et al. 2007
Variable Stars in I Zw 18
Lowest metallicity Cepheids
ever observed !
Z = 1/50 Zo
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125 days
8.6 days
130 days
139 or 186 days
Variable Stars in I Zw 18
Lowest metallicity Cepheids
ever observed !
Z = 1/50 Zo
12
125 days
8.6 days
130 days
139 or 186 days
Aloisi et al. 2007
P = 8.6 days
Distance of I Zw 18
• Cepheids – theoretical reddening-free Wesenheit relation for the 3 confirmed Cepheids yields average distance D = 19 ± 2 Mpc
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Distance of I Zw 18
• Cepheids – theoretical reddening-free Wesenheit relation for the 3 confirmed Cepheids yields average distance D = 19 ± 2 Mpc
• TRGB – TRGB filtering technique gives D = 18 ± 2 Mpc
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Distance of I Zw 18
• Cepheids – theoretical reddening-free Wesenheit relation for the 3 confirmed Cepheids yields average distance D = 19 ± 2 Mpc
• TRGB – TRGB filtering technique gives D = 18 ± 2 Mpc
Distance larger than previously believed; contributed to difficulty in detecting RGB
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PL Relation vs. Metallicity
Fiorentino et al. 2007 (to be submitted)
Closer metal-poor BCDs need to be additionally investigated in order to better constrain PL relation at low metallicity
Several BCDs available within the Local Volume !14
HST UV Spectroscopy after SM4
Aloisi et al. 2003
COS & STIS will allow studies of the neutral ISM in star-forming systems (e.g., FUSE study of I Zw 18)
In particular, COS will be crucial in the FUV
to characterize the realO abundances from the 1300-
1350 Å region
Confirmation of the metallicity offset between neutral and ionized gas ?
Constraints to chemical evolution models
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