Field-of-view sacrificed to ensure schedulability with two-gyros.
----- Submission 1 (Thu May 04 15:54:54 GMT 2006) -----
Phase II Proposal 10835 (10835_N4278_N3379_2) successfully submitted.
----- Submission 2 (Tue Aug 01 21:07:51 GMT 2006) -----
Phase II Proposal 10835 (10835_N4278_N3379_2_ICRS) successfully submitted.
----- Submission 3 (Tue Aug 08 16:21:03 GMT 2006) -----
Assigned ID: 392
----- Submission 1 (Fri Jan 27 20:30:57 GMT 2006) -----
Phase I Proposal 392 (N4278_3379) successfully submitted.
Probing The Globular Cluster / Low Mass X-ray Binary Connection in Early-type Galaxies At Low X-ray Luminosities
Combined high-resolution imaging from Hubble and Chandra (CXO) has revolutionized our understanding of extragalactic low-mass X-ray binaries (LMXBs) and globular clusters (GCs), yet their connection in early-type galaxies has remained unstudied at the luminosities of the Galactic LMXBs in GCs. NGC 4278 and 3379 will be the first two prototypical elliptical galaxies with deep CXO observations enabling the study of LMXBs at lower luminosities. We propose mosaic ACS observations of both galaxies (5 fields per galaxy) that will provide the most comprehensive view into the connection between GCs and LMXBs in early-type galaxies. We will detect ~860 and ~270 GCs in all of NGC 4278 and NGC 3379, respectively. These two galaxies will have among the greatest number of detected GC-LMXBs to date (~130 & 50) and will include the faintest GC-LMXBs in a normal early-type galaxy. We will measure the fraction of GCs which contain LMXBs, as a function of X-ray luminosity, galactocentric distance, color, and GC half-light radius. Using the radial profiles of optical light, GCs, and LMXBs, we will determine the percentage of field LMXBs which may have originated in GCs. We will use the measured GC properties over the entire extent of both galaxies to constrain theories of GC formation and evolution.
Our science goal is to obtain a nearly complete census of globular clusters in NGC 3379 and NGC 4278, and make comparisons to the low-mass X-ray binary population using the ACS/WFC. For each galaxy, we will perform a 2x2 mosaic plus an additional central field to cover beyond the isophotal 25 mag arcsec^-2 surface. We will observe the central fields in F475W for 676s total exposure and in F850LP for 1150s total exposure using 2-point hot-pixel dither patterns plus a 90s exposure to avoid saturation at the galaxy center. For the 2x2 mosaic fields (accomplished by POS_TARG offsets from the central fields), we will observe in F475W for 702s total exposure using a 2-point hot-pixel dither pattern and in F850LP for 1200s total exposure using a 3-point hot-pixel dither pattern. Our chosen dither patterns optimize the rejection of hot pixels and cosmic rays while maximizing total exposure time. NGC 3379 is schedulable for 113 days, while NGC 4278 is schedulable for 122 days.
The 2x2 mosaic fields are currently constrained to have the same orientation as the central field. This requirement could be relaxed if scheduling difficulties arise.
UNRESOLVED STELLAR POPULATIONS
12
false
0.0
false
false
false
false
false
SUPPORTED
GALAXY
ELLIPTICAL
This object was generated by the targetselector and retrieved from the NED database.
V=23.6, magnitude is that of a typical globular cluster in NGC 4278
J2000
12 20 6.0000
+29 16 53.28
J2000
GALAXY
ELLIPTICAL
This object was generated by the targetselector and retrieved from the NED database.
V=22.9, magnitude is that of a typical globular cluster in NGC 3379
J2000
10 47 48.9000
+12 34 57.14
J2000
ACS/WFC
Imaging
No
No
F475W
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No
No
F850LP
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No
No
F475W
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F850LP
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F475W
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F475W
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F475W
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Imaging
No
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F850LP
POS-TARG
DITHER
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LINE
false
false
2
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ACS-WFC-DITHER-LINE
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false
POS-TARG
DITHER
0.145
LINE
false
false
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ACS-WFC-DITHER-LINE
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