----- Submission 1 (Tue May 13 21:55:13 GMT 2003) -----
----- Submission 2 (Wed Jul 16 21:24:02 GMT 2003) -----
Successfully submitted: Wed Jul 16 21:24:05 GMT 2003
----- Submission 3 (Fri Jul 18 19:25:40 GMT 2003) -----
Search for Black Holes in M31 Globular Clusters
Whether globular clusters contain a central massive black hole remains
a very controversial subject today, and yet is extremely important for
theoretical models for black hole and cluster formation. Furthermore,
the existence of intermediate-mass black holes has important implications
for supermassive black hole and galactic bulge formation, as well as
providing signatures in gravitational wave detectors. We propose to obtain
high spatial resolution, long-slit spectroscopy of two globular clusters in
M31, G78 and G280. These two clusters represent the best ones in which to
constrain a central black hole. Most importantly, both of these clusters have
long central relaxation times, and thus confusion between a central black
hole and a collection of heavy stellar remnants is alleviated. We have
considered all globular clusters in our Galaxy and in M31; STIS observations
of these two will provide the strongest limits for a black hole in any cluster,
and better than the two claims made previously in the literature. Combined
with the data for G1, these three clusters have the three highest central
velocity dispersions for any cluster in the Local Group and will shed light
on possible connections between galaxy and globular cluster formation.
From the STIS exposure time calculator, our simulations, and our
previous experience with G1 and M33, we can very accurately calculate
the necessary exposure times. The central surface brightness of G78 is
$\mu_V$ = 14.2 mag arcsec$^{-2}$ (Fusi Pecci et al. 1994), and for
G280 it is $\mu_V$ = 15 mag arcsec$^{-2}$ (Dubath \& Grillmair
1997). Both of these central surface brightness profiles are estimates
since there has not been post-repair {\it HST}\ imaging for
either. Our estimates come from King model fits to the outer radii;
these fits tend to slightly underestimate the amount of light in the
central regions (Noyola \& Gebhardt 2003, in preparation) and so we
have conservatively chosen the value as derived from King fits. To
reach a S/N = 40 per resolution element (two spatial 0.05\arcsec\ STIS
pixels) at 8500 \AA\ with the 52x0.1 slit requires 360 minutes for G78
and 750 minutes for G280. However, the dispersion profile out to
$\sim$1.0\arcsec\ is important for the dynamical analysis.
Fortunately, we only require an accuracy of 15\% for the dispersion
profile at this radius, which implies that we only need to attain S/N
= 35. Both G78 and G280 have relatively low concentration and core
radii $\sim$0.5\arcsec. Thus, there is not much decrease in the
surface brightness profile out to 1\arcsec. Since we can also sum over
at least four STIS pixels at these radii, the dispersion uncertainty
remains relatively constant as a function of radius for a given
exposure time.
We also request ACS/HRC observations for both of these clusters and
for G1. There is no post-repair {\it HST}\ imaging for either G78 or
or G280, and the surface brightness profile is essential to help
constrain the dynamical models. The previous WFPC2 observations of G1
were not optimized for measuring the central profile well. We will
take multiple dither positions in order to provide to best spatial
resolution possible. For each cluster, one orbit is adequate given
their high central surface brightnesses.
For G78, we request 9 STIS orbits (including overhead) and 1 ACS
orbit. For G280, we request 17 STIS orbits (including overhead) and 1
ACS orbit. For G1, we request 1 ACS orbit. The total orbit request is
29.
GALAXIES
12
false
false
false
false
SUPPORTED
STELLAR CLUSTER
GLOBULAR CLUSTER
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
J2000
STELLAR CLUSTER
GLOBULAR CLUSTER
J2000
00 41 1.4
+41 13 46.0
J2000
STIS/CCD
ACCUM
Spectroscopic
No
STIS/CCD
ACCUM
00 44 29.8
+41 21 36.0
J2000
STIS/CCD
ACCUM
Spectroscopic
No
STIS/CCD
ACCUM
00 41 1.4
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J2000
ACS/HRC
ACCUM
Imaging
No
ACS/HRC
ACCUM
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J2000
ACS/HRC
ACCUM
Imaging
No
ACS/HRC
ACCUM
00 32 46.6
+39 34 40.0
J2000
ACS/HRC
ACCUM
Imaging
No
ACS/HRC
ACCUM
00 41 1.4
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J2000
ACS/WFC
ACCUM
Imaging
No
ACS/WFC
ACCUM
00 44 29.8
+41 21 36.0
J2000
ACS/WFC
ACCUM
Imaging
No
ACS/WFC
ACCUM
false
false
ACS-HRC-DITHER-LINE
false
44.28
1
0.131
DITHER
3
LINE
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