The Stellar Halo Profiles of Massive Disk Galaxies
Stellar halos surrounding massive galaxies are of prime interest in hierarchical galaxy
formation models: most of the halo is formed by the very early accretion of small, metal
poor satellite galaxies each with their independent evolution history. As such, halos
contain the fossil remnants of the earliest star formation and accretion phases of a
galaxy in formation. The resulting size, shape, age, and metallicity of stellar halos
provide therefore a direct test of the basic ingredients (reionization, feedback from star
formation, density fluctuation power spectrum) of hierarchical galaxy formation models.
In our GHOSTS survey we have sampled the principle axes of a sample of 11 nearby galaxies
with Vrot>100 km/s. Our detection of resolved stellar halo populations ~1.5 mag below the
tip of the Red Giant Branch has revealed halos that extend as far as 30 kpc around the
most massive galaxies in our sample. Those extended stellar halos seem more compact than
current model predictions, they have unexpectedly high metallicity up to the last detected
point, and have a luminosity that is more closely related to the bulge luminosity than to
the galaxy mass. We propose to extend the light profiles of 4 massive galaxies with a
range in bulge-to-disk ratio to the background limit at ~70 kpc. This will enable us to:
- confirm the stellar halo shape (compactness) and assess with confidence any conflict
with models using these very extended and accurate halo profile characterizations;
- establish whether stellar envelopes beyond 30 kpc are still morphologically connected to
inner bulges, or whether a break occurs at larger radii revealing a distinct new component;
- determine whether every massive galaxy has an old, metal-poor halo at large radius
like the Milky Way and M31; if not, constrain for the first time the range of stellar
metallicity gradients in extended stellar halos.
To measure metallicities from the RGB colors, we need to reach 1.0 mag below the tip of the RGB, which occurs almost independent of metallicity at m_I=−4 mag andw ith V−I~1. We have used the ETC and our GHOSTS experience to calculate the required exposure times for optimal PSF fit photometry in Low Sky conditions, based on GHOSTS TRGB distances. Dithering between orbits, we will typically expose 800s and 1400s per orbit in F606W and F814W with WFC3, and 1100s and 1000s with ACS.
We use POSTARGS to do the dithering, as this gives us the largest flexibility to determine offsets and to pack the orbits efficiently with the ACS & WFC3 parallels. The POSTARGS also put the apertures outside the target position, but this is done on purpose such that the rotation point where the ACS and WFC3 parallel rotate around is in between the two cameras and the positional shift remains small for both cameras independent of the final ORIENT chosen.
COSMOLOGY
12
false
0.0
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false
false
false
false
false
false
SUPPORTED
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
GALAXY
HALO
SPIRAL
This object was generated by the targetselector and retrieved from the NED database.
J2000
00 47 33.1000
-25 17 18.00
J2000
26 I-mag
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
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Same orient constraint links visits (21 22 23)
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Same orient constraint links visits (21 22 23)
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:si-bright-earth-limb-angle 40.0
:data-volume 2291872
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 12213
:visit-id "34"
:obset-id "34"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 12213
:visit-id "34"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2620
:al-overhead-at-end 116
:internal-dur-at-end 0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "Y"
:pcs-visibility 3191
:pcs-gap 401
)
(Tic-Orbit
:proposal-id 12213
:visit-id "34"
:orbit-number 2
:pcs-time 222
:si-vis-utilization 2620
:al-overhead-at-end 116
:internal-dur-at-end 1019
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "Y"
:pcs-visibility 3191
:pcs-gap 401
)
true
2
0