# Spectral energy distributions and age estimates of 104 M31 globular clusters

Song Wang,11affiliation: National Astronomical Observatories, Chinese Academy
of Sciences, Beijing, 100012, P. R. China;
<EMAIL_ADDRESS>22affiliation: Graduate University, Chinese Academy of
Sciences, Beijing, 100039, P. R. China 33affiliation: Key Laboratory of
Optical Astronomy, National Astronomical Observatories, Chinese Academy of
Sciences, Beijing, 100012, China Zhou Fan,11affiliation: National Astronomical
Observatories, Chinese Academy of Sciences, Beijing, 100012, P. R. China;
<EMAIL_ADDRESS>Jun Ma,11affiliation: National Astronomical
Observatories, Chinese Academy of Sciences, Beijing, 100012, P. R. China;
<EMAIL_ADDRESS>33affiliation: Key Laboratory of Optical Astronomy,
National Astronomical Observatories, Chinese Academy of Sciences, Beijing,
100012, China Richard de Grijs,44affiliation: Kavli Institute for Astronomy
and Astrophysics, Peking University, Beijing, 100871, P. R. China
55affiliation: Department of Physics & Astronomy, University of Sheffield,
Sheffield S3 7RH, UK Xu Zhou11affiliation: National Astronomical
Observatories, Chinese Academy of Sciences, Beijing, 100012, P. R. China;
<EMAIL_ADDRESS>
###### Abstract

We present photometry of 104 M31 globular clusters (GCs) and GC candidates in
15 intermediate-band filters of the Beijing-Arizona-Taiwan-Connecticut (BATC)
photometric system. The GCs and GC candidates were selected from the Revised
Bologna Catalog (v.3.5). We obtain the cluster ages by comparing the
photometric data with up-to-date theoretical synthesis models. The photometric
data used are GALEX far- and near-ultraviolet and 2MASS near-infrared
$JHK_{\rm s}$ magnitudes, combined with optical photometry. The ages of our
sample clusters cover a large range, although most clusters are younger than
10 Gyr. Combined with the ages obtained in our series of previous papers
focusing on the M31 GC system, we present the full M31 GC age distribution.
The M31 GC system contains populations of young and intermediate-age GCs, as
well as the ‘usual’ complement of well-known old GCs, i.e., GCs of similar age
as the majority of the Galactic GCs. In addition, young GCs (and GC
candidates) are distributed nearly uniformly in radial distance from the
center of M31, while most old GCs (and GC candidates) are more strongly
concentrated.

###### Subject headings:

galaxies: individual (M31) – galaxies: star clusters – galaxies: stellar
content

††slugcomment: AJ, in press

##  1\. Introduction

Globular clusters (GCs) are among the oldest known stellar systems in the
Universe. They typically have ages similar to those of their host galaxies,
thus making them fossils that may provide important information about the
formation and evolution of their parent galaxies. In addition, nearly all
types of galaxies contain GCs, from dwarfs to giants and from the earliest to
the latest types (Fusi Pecci et al., 2005). However, our most in-depth
understanding of GC systems has predominantly come from studies of the Milky
Way.

M31, located at a distance of $\sim 780$ kpc (Stanek & Garnavich, 1998; Macri,
2001), is the largest galaxy in the Local Group. By virtue of the natural
advantage of being located at a reasonable distance, the galaxy offers us an
ideal environment for detailed, resolved investigations of a large GC system,
using both Hubble Space Telescope (HST) (e.g., Grillmair et al., 1996; Holland
et al., 1997; Rich et al., 2005; Perina et al., 2009b) and ground-based
observations with large telescopes (e.g., Christian & Heasley, 1991).

A large number of studies focusing on the M31 GC system have been performed
since Hubble (1932)’s original identification of 140 GC candidates in M31. The
latest Revised Bologna Catalogue of M31 GCs and candidates (hereafter RBC
v.3.5) (Galleti et al., 2004, 2006, 2007) was updated on March 27, 2008, and
contains 1983 objects (509 confirmed and 1049 candidate GCs, 9 controversial
objects, 147 galaxies, 6 Hii regions, 245 stars, 5 asterisms, and 13 extended
clusters). These objects were observed and discovered by a large number of
authors using a variety of observational systems (see, e.g., Vetes̆nik, 1962;
Sargent et al., 1977; Battistini et al., 1980; Crampton et al., 1985; Barmby
et al., 2000). To obtain a homogeneous photometric data set, Galleti et al.
(2004) took the observed data of Barmby et al. (2000) as reference and
transformed other observations to this standard setup.

An accurate and reliable analysis of star clusters is important for our
understanding of the formation, buildup, and evolutionary processes in
galaxies. By comparing integrated photometry with models of simple stellar
populations (SSPs), recent studies have achieved some success in determining
ages and masses of extragalactic star clusters (e.g., de Grijs et al., 2003a,
b, c; de Grijs & Anders, 2006; Bik et al., 2003; Ma et al., 2006a; Fan et al.,
2006; Ma et al., 2007a, 2009a). Ma et al. (2006a) and Fan et al. (2006)
derived age estimates for M31 GCs by fitting SSP models (Bruzual & Charlot,
2003, henceforth BC03) to their photometric measurements in a large number of
intermediate- and broad-band filters spanning the spectral range from the
optical to the near-infrared (NIR). In particular, Ma et al. (2007a)
determined an age for the M31 GC S312 (B379), using multicolor photometry from
the near-ultraviolet (near-UV) to the NIR, of $9.5^{+1.2}_{-1.0}$ Gyr. S312
(B379) is, in fact, among the first extragalactic GCs for which the age was
estimated accurately and independently, using main-sequence photometry, at
$10^{+2.5}_{-1}$ Gyr (Brown et al., 2004). This provides a robust check on our
methodology to derive age constraints based on the spectral energy
distributions (SEDs) of (simple) stellar systems.

This paper is organized as follows. In §2 we present Beijing-Arizona-Taiwan-
Connecticut (BATC) observations of our sample GCs and GC candidates, the
relevant data-processing steps, and the GALEX (far- and near-UV), optical
broad-band, and Two-Micron All Sky Survey (2MASS) NIR data that are
subsequently used in our analysis. In §3 we derive the ages of our sample
clusters by comparing their SEDs with the galev SSP models. We then discuss
and summarize our results in §4.

##  2\. GC sample and BATC intermediate-band photometry

###  2.1. GC sample selection

To obtain photometry in 15 intermediate-band filters of the BATC photometric
system for 61 GCs and GC candidates in the RBC v.3.5, for which few
measurements are presently available in any photometric system, Fan et al.
(2009) mined the BATC survey archive for observations obtained between
February 1995 and March 2008. The resulting set of observations covers
approximately six square degrees. For the purpose of estimating accurate
cluster ages, we selected clusters for which the metallicities and reddening
values had been estimated accurately, independently, and homogeneously in
previous studies (Huchra et al., 1991; Barmby et al., 2000; Perrett et al.,
2002; Fan et al., 2008): see §2.6. We selected classes 1, 2, 3, and 8 (1580
objects) from column ‘f’ in the RBC v.3.5, which include GCs, candidate GCs,
controversial objects, and extended clusters. This resulted in an initial
selection of 366 objects. Jiang et al. (2003), Ma et al. (2006a), and Ma et
al. (2009a) obtained multicolor photometry for 180 of these GCs and GC
candidates. In this paper, we consider the remaining 186 objects. Caldwell et
al. (2009) published an updated catalog of 1300 objects in M31, including 670
likely star clusters, with the remaining objects being stars or background
galaxies once thought to be clusters (see Tables 3 and 5 of Caldwell et al.,
2009). From a comparison with Caldwell et al. (2009), we find that 66 objects
are either stars or background galaxies. Therefore, the final sample of M31
GCs and GC candidates analyzed in this paper includes 120 objects. However, we
cannot obtain accurate photometric measurements for 16 of these objects
because of either a nearby very bright object (B065 and B344D), very faint
fluxes superimposed onto a bright background (B119, B396, NB16, and V031), or
a location very close to (or blend with) another object (B150D, B176, B256D,
B302, B345, B366, B381, B391, and B397), leading to compromised photometric
measurements. Object B330 is both faint and located very close to a brighter
object. Thus, here we analyze the multicolor photometric properties of 104 GCs
and GC candidates. Figure 1 shows their spatial distribution across the M31
fields observed with the BATC multicolor system.

Figure 1.— BATC observations of our M31 fields. Each field is $58\arcmin\times
58\arcmin$ (size of the old CCD). The large ellipse is the boundary between
the M31 disk and halo (Racine, 1991), while the two small ellipses represent
the $D_{25}$ isophotes of NGC 205 (northwest) and M32 (southeast). Solid
circles indicate the sample GCs and GC candidates discussed in this paper.

###  2.2. BATC intermediate-band photometry

The observations of our sample GCs and GC candidates were carried out in the
BATC photometric system, using the 60/90 cm $f$/3 Schmidt telescope at
Xinglong Station of the National Astronomical Observatories of the Chinese
Academy Sciences (NAOC). The BATC system includes 15 intermediate-band
filters, covering a wavelength range from 3300 Å to 1 $\mu$m. The parameters
of the filters are given in Table 1, where column (1) gives the filter name,
column (2) is the central wavelength for each filter, and column (3) lists the
bandwidth for each filter. The 2k$\times$2k CCD used before February 2006 had
a pixel size of 15 $\mu$m and a resolution of $1.7^{\prime\prime}$ pixel-1.
After February 2006, a new 4k$\times$4k CCD with a pixel size of 12 $\mu$m was
used, with a resolution of $1.3^{\prime\prime}$ pixel-1 (Fan et al., 2009).
The new CCD camera is much more sensitive at short wavelengths.

We obtained 143.9 hours of imaging (447 images) of the M31 field, covering
about six square degrees, through the set of 15 filters in five observing runs
from 1995 to 2008, spanning 13 years (see for details Fan et al., 2009). The
data were reduced using standard procedures, including bias subtraction and
flat fielding of the CCD images, with an automatic data-reduction software
package (PIPELINE I) specifically developed for the BATC sky survey. BATC
magnitudes are defined and obtained in a similar way as for the
spectrophotometric AB magnitude system (see for details Ma et al., 2009a). For
the $a$ to $p$ filters of the central field of M31 (M31-1 in Figure 1), the
absolute flux of the combined images was obtained using calibrated standard
stars, while for the M31-2 to M31-7 fields we used the M31-1 field to derive
secondary transformations (see for details Fan et al., 2009).

We determined the magnitudes of our sample objects on the combined images
using standard aperture photometry, i.e., using the PHOT routine in DAOPHOT
(Stetson, 1987). To avoid contamination from nearby objects, we adopted
apertures with radii of 3 and 4 pixels on the 2k$\times$2k and 4k$\times$4k
CCDs, respectively. For the old CCD, we took 8 and 13 pixels from the object’s
center as the inner and outer radii of the sky annulus for background
determination, while for the new CCD, the corresponding radii were set at 10
and 17 pixels, respectively (Fan et al., 2009). We used isolated stars to
obtain point-source aperture corrections by measuring the magnitude
differences between the fluxes contained within radii of 3 (4) pixels on the
old (new) CCD images and the total stellar magnitudes in each of the 15 BATC
filters. The resulting aperture-corrected SEDs for the sample GCs and GC
candidates in M31 are provided in Table 2. Columns (2) to (16) represent the
magnitudes in the 15 BATC passbands used for our photometry. The $1\sigma$
magnitude uncertainties, from DAOPHOT, are listed for each object on the
second line for the corresponding passband. For some GCs and GC candidates,
the magnitudes in some filters could not obtained because of low signal-to-
noise ratios.

###  2.3. GALEX UV, optical broad-band, and 2MASS NIR photometry

To estimate the ages of the M31 GCs and GC candidates, we should ideally use
as many photometric data points covering as wide a wavelength range as
possible (cf. de Grijs et al., 2003b; Anders et al., 2004; Ma et al., 2009a).
The RBC v.3.5 includes GALEX (far- and near-UV) fluxes from Rey et al. (2007),
optical broad-band, and 2MASS NIR magnitudes for 1983 objects, which we use as
the basis for our analysis. Although the $UBVRI$ magnitudes of the objects
published by Barmby et al. (2000) are included in the RBC v.3.5 and as such
provide the most homogeneous set of photometric measurements available, the
relevant photometric uncertainties are not listed. Therefore, we adopt the
original $UBVRI$ measurements of Barmby et al. (2000), including their
published photometric errors. For the remaining objects we adopt the $UBVRI$
measurements from the RBC v.3.5. We assign photometric uncertainties following
Galleti et al. (2004), i.e., $\pm 0.05$ mag in $BVRI$ and $\pm 0.08$ mag in
$U$ (see for details Ma et al., 2009a).

In the RBC v.3.5, the 2MASS $JHK_{\rm s}$ magnitudes were transformed to the
CIT photometric system (Galleti et al., 2004). However, we need the original
2MASS $JHK_{\rm s}$ data to compare the observed SEDs with the SSP models, so
we reversed the transformation using the equations given by Carpenter (2001).
We obtained the magnitude errors in the $JHK_{\rm s}$ bands by comparing our
photometric data with fig. 2 of Carpenter et al. (2001), which shows the
generic photometric uncertainties as a function of magnitude for stars
brighter than their observational completeness limits (see for details Ma et
al., 2009a). We include the GALEX, optical broad-band, and 2MASS NIR
photometry of the sample clusters in Table 3 (columns 3 to 12), where the
photometric errors are listed for each object on the second line for the
corresponding passband. The GALEX photometric system is calibrated to match
the spectrophotometric AB system, while the optical broad-band and 2MASS
photometric data are given in Vega magnitudes. Finally, column 2 includes the
classification flags from the RBC v.3.5.

###  2.4. Comparison with previously published photometry

To check our photometry, we transformed the BATC intermediate-band system to
the $UBVRI$ broad-band system using the relationships between these two
systems derived by Zhou et al. (2003):

$B=m_{d}+0.2201(m_{c}-m_{e})+0.1278\pm 0.076\quad\mbox{and}$ (1)

$V=m_{g}+0.3292(m_{f}-m_{h})+0.0476\pm 0.027.$ (2)

$B$-band photometry can be derived from the BATC $c,d$, and $e$ bands, while
$V$-band magnitudes can be obtained from the BATC $f,g$, and $h$ bands. Figure
2 shows a comparison of the $B$ and $V$ photometry of our M31 sample objects
with previous measurements from Barmby et al. (2000) and Galleti et al.
(2004). The mean $B$ and $V$ magnitude differences—in the sense of this paper
minus Barmby et al. (2000) or Galleti et al. (2004)—are $\langle\Delta
B\rangle=-0.077\pm 0.022$ mag and $\langle\Delta V\rangle=-0.047\pm 0.033$.
Our magnitudes are in good agreement with previous $V$-band determinations.
However, a significant disagreement becomes apparent in the $B$ band for
objects with $B>17.5$ mag. This disagreement has its origin in the difference
between our photometry and that of Galleti et al. (2004). In fact, our
$B$-band photometry agrees well with that of Barmby et al. (2000), even for
$B>17.5$ mag objects (except for one sample cluster). Referring to Jiang et
al. (2003) and Ma et al. (2009a), we also see that our photometric values are
fully consistent with Barmby et al. (2000). In Ma et al. (2009a), the analysis
of the majority of the GCs was based on the photometric data of Barmby et al.
(2000), so even in the $B$ band the agreement is good: see fig. 3 of Ma et al.
(2009a). We excluded B257 from the comparison, because its $V$-band magnitude
is too faint compared with the magnitudes obtained in the other bands (see
Table 3). In fact, from the observed SEDs, this photometric measurement is
unusually far away from the best-fitting integrated SEDs (see §3 for more
details). This data point was taken from Table 4 of Barmby & Huchra (2001),
and the offset may be a typical error. Based on the BATC $f,g$, and $h$
magnitudes, we obtain $V=17.76$ mag for B257. Note that the $B$-band magnitude
of this cluster as listed in Table 4 of Barmby & Huchra (2001) is 11.907,
which is too bright for any reasonable SED and may also be a typical
uncertainty.

Figure 2.— Comparison of the photometry of our GCs and GC candidates with
previous measurements from Barmby et al. (2000) (triangles) and Galleti et al.
(2004) (crosses). The dashed lines enclose $\Delta V$ and $\Delta B=0.3$ mag.

###  2.5. Metallicities and reddening values

We require independently (but homogeneously) determined metallicities and
reddening values to robustly and accurately estimate the ages of our sample
objects. We used three homogeneous sources of spectroscopic metallicities
(Huchra et al., 1991; Barmby et al., 2000; Perrett et al., 2002) and one
homogenized reference (see for details Fan et al., 2008; Ma et al., 2009a).

Following Ma et al. (2009a), for reasons of consistency we ranked the sources
used to assign metallicities to our M31 GCs in order of preference.
Metallicities from Perrett et al. (2002) were chosen whenever available
because of the large number of their metallicity determinations, followed (in
order) by metallicity determinations from Barmby et al. (2000) and Huchra et
al. (1991). If none of these three sources included spectroscopic
metallicities for a given sample cluster, we used the corresponding value from
Fan et al. (2008).

For reddening values, we used Barmby et al. (2000) and Fan et al. (2008) as
our reference (see for details Ma et al., 2009a). Because the reddening values
from Fan et al. (2008) comprise a homogeneous data set and the number of GCs
included is greater than that of Barmby et al. (2000), we preferentially adopt
Fan et al. (2008) reddening values, followed by those of Barmby et al. (2000),
in a similar approach as adopted by Ma et al. (2009a). The metallicities and
reddening values adopted for our sample clusters are listed in Table 4.

##  3\. Age determination

An SSP is defined as a single generation of coeval stars characterized by the
same parameters, including metallicity, age, and stellar initial mass function
(IMF). SSP models are calculated on the basis of a set of evolutionary tracks
of stars of different initial masses, combined with stellar spectra at
different evolutionary stages. In this paper, and following Ma et al. (2009a),
we compare the SEDs of our sample objects with the galev SSP models (e.g.,
Kurth et al., 1999; Schulz et al., 2002; Anders & Fritze-v. Alvensleben, 2003)
to estimate their ages. The galev SSPs are based on the Padova isochrones
(covering wavelengths from 91 Å to 160 $\mu$m) and a Salpeter (1955) stellar
IMF with lower and upper mass limits of $0.10~{}{\rm M}_{\odot}$ and 50–70
${\rm M}_{\odot}$, respectively (the latter depending on metallicity). These
models cover ages from 4 Myr to 16 Gyr, with an age resolution of 4 Myr for
ages younger than 2.35 Gyr, and 20 Myr for older ages. We convolved the
theoretical SSP SEDs with the GALEX, broad-band $UBVRI$, BATC intermediate-
band, and 2MASS $JHK_{\rm s}$ filter response curves to obtain synthetic UV,
optical, and NIR photometry (Ma et al., 2009a). The synthetic magnitude in the
AB magnitude system for the $i^{\rm th}$ filter is

$m_{i}=-2.5\log\frac{\int_{\nu}F_{\nu}\varphi_{i}(\nu){\rm
d}\nu}{\int_{\nu}\varphi_{i}(\nu){\rm d}\nu}-48.60,$ (3)

where $F_{\nu}$ is the theoretical SSP SED (which is a function of age and
metallicity) and $\varphi_{i}$ is the response curve of the $i^{\rm th}$
filter. The galev SSP models include five initial metallicities,
$Z=0.0004,0.004,0.008,0.02$ (solar), and $0.05$. For other metallicities, the
relevant spectra can be obtained by linear interpolation of the appropriate
model spectra for any of these five metallicities. For metallicities below
$Z=0.0004$ we use the $Z=0.0004$ model (Ma et al., 2009a).

To determine the most compatible galev SSP model for a given observed SED, we
adopted a $\chi^{2}$ minimization test,

$\chi^{2}=\sum_{i=1}^{25}{\frac{[m_{\nu_{i}}^{\rm intr}-m_{\nu_{i}}^{\rm
mod}(t)]^{2}}{\sigma_{i}^{2}}},$ (4)

where $m_{\nu_{i}}^{\rm mod}(t)$ is the magnitude in the $i^{\rm th}$ filter
of a theoretical SSP at age $t$, while $m_{\nu_{i}}^{\rm intr}$ is the
intrinsic (observed and corrected) magnitude in the same filter. The
interstellar extinction curve $A_{\nu}$ is taken from Cardelli et al. (1989),
$R_{\nu}=A_{V}/E_{B-V}=3.1$. $\sigma_{i}$ is the magnitude uncertainty in the
$i^{\rm th}$ filter, defined as

$\sigma_{i}^{2}=\sigma_{{\rm obs},i}^{2}+\sigma_{{\rm mod},i}^{2}.$ (5)

Here, $\sigma_{{\rm obs},i}$ and $\sigma_{{\rm mod},i}$ are the observational
uncertainty and that associated with the model itself, respectively. Charlot
et al. (1996) estimated $\sigma_{{\rm mod},i}$ by comparing the colors
obtained from different stellar evolutionary tracks and spectral libraries. We
adopt $\sigma_{{\rm mod},i}=0.05$ mag, following Wu et al. (2005), Ma et al.
(2006a, 2009a), and Fan et al. (2006). The SED fits of our sample GCs and GC
candidates are shown in Fig. 3.

Figure 3.— SED fits of the galev SSP models to our sample objects.

Figure 3.— Continued.

Figure 3.— Continued.

##  4\. Results and summary

In §3 we determined the ages of 104 GCs and GC candidates in M31. The results
are tabulated in Table 5. Figure 4 shows the age distribution of the sample
clusters, from which we conclude that, except for 20 clusters, the ages of
most sample GCs are between 1 and 5 Gyr, with a peak at $\sim 2$ Gyr. The
‘usual’ complement of well-known old GCs (i.e., GCs of similar age as the
majority of the Galactic GCs) is also present. In addition, while fitting SSP
models to the observed data, we found that some photometric data of a small
number of clusters cannot be fitted with any SSP models. We therefore did not
use these deviating photometric data points to obtain the best fits. This
applies to the GALEX far-UV data of B138D, the 2MASS $K_{\rm s},H$, and $J$
magnitudes of B142D, B181D, and B289D, respectively, the $B$-band and 2MASS
$H$ fluxes of B245D, and the $V$-band magnitude of B257.

Other authors have also considered the age distribution of the GCs in M31. For
example, Barmby et al. (2000) discovered that M31 contains GCs exhibiting
strong Balmer lines and A-type spectra, from which one infers that these
objects must be very young. Beasley et al. (2004) and Puzia et al. (2005)
confirmed this conclusion. Burstein et al. (2004) and Fusi Pecci et al. (2005)
carefully studied the sample of young M31 GCs. Very recently, Caldwell et al.
(2009) determined the ages and reddening values of 140 young clusters in M31
by comparing the observed spectra with models, and found that these clusters
are less than 2 Gyr old, while most clusters have ages between $10^{8}$ and
$10^{9}$ yr. Perina et al. (2009a) estimated an age for VDB0-B195D of $\sim
25$ Myr based on HST/WFPC2 color-magnitude diagrams (CMDs). The ages of the
M31 clusters determined in this paper are in general agreement with previous
determinations, which we will show in more detail below on the basis of
comparisons between our determinations and previous age estimates for
individual objects.

The most direct and most accurate method to determine a cluster’s age is by
means of main-sequence photometry, since the absolute magnitude of the main-
sequence turnoff is a strong function of age. Williams & Hodge (2001a, b)
estimated ages of many young disk clusters in M31 based on HST/WFPC2 CMDs and
isochrone fitting to either the main sequence or luminous evolved stars. Only
one of their clusters (B315) is in common with our sample. They obtained an
age of $\sim 0.1$ Gyr for this cluster, while we determined it to be
approximately 0.5 Gyr old. Both age determinations are mutually consistent
within the uncertainties. Caldwell et al. (2009) compared their ages with
those of Williams & Hodge (2001a, b) and concluded that both sets of age
determinations were in good agreement. We therefore compare our ages with
Caldwell et al. (2009) for the seven clusters we have in common with their
sample (B018, B307, B316, B448, B475, B483, and V031: see Table 6). It is
evident that they are largely internally consistent. Puzia et al. (2005) also
presented spectroscopic ages, metallicities, and ${\rm[\alpha/Fe]}$ ratios for
70 M31 GCs based on Lick line-index measurements. A cross correlation with
Puzia et al. (2005)’s sample shows that we have 21 clusters in common. A
direct comparison shows that the ages of Puzia et al. (2005) are
systematically older than ours. This surprising result prompted us to compare
the ages of clusters in common between Puzia et al. (2005) and other authors
(Williams & Hodge, 2001a, b; Beasley et al., 2004; Caldwell et al., 2009). We
found similar systematic offsets (see for details also Ma et al., 2009a).

Figure 4.— Age distribution of our sample GCs and GC candidates in M31.

We have determined the ages of M31 GCs and GC candidates in a series of
previous papers (Jiang et al., 2003; Ma et al., 2006a, b; Fan et al., 2006; Ma
et al., 2007a, 2009a, 2009b) based on the same method as used in the present
paper, i.e., by constructing SEDs of known M31 GC candidates and using the SED
shapes to estimate cluster ages. In the first paper of this series, Jiang et
al. (2003) estimated the ages of 172 M31 GC candidates based on photometric
measurements in 13 BATC intermediate-band filters and the SSP models of
Bruzual & Charlot (1996; unpublished, hereafter BC96). Subsequently, Fan et
al. (2006) obtained new age estimates for 91 GCs from the Jiang et al. (2003)
sample, based on improved photometric data including intermediate- and broad-
band magnitudes from the optical to the NIR, and the SSP models of BC03. Ma et
al. (2006b) then estimated the ages of 33 M31 GC candidates using photometry
in 13 BATC intermediate-band filters and the BC03 SSP models, while Ma et al.
(2009a) determined the ages of 35 M31 GCs and GC candidates based on
photometry including far- and near-UV GALEX observations, $UBVRI$, 13 BATC
intermediate-band filters, and 2MASS $JHK_{\rm s}$, combined with the galev
SSP models. Ma et al. (2006a, 2007a, 2009b) determined the ages of three
specific M31 GCs (037-B327, S312, and G1) based on the BC03 SSP models and a
large number of photometric measurements. We determined the ages of these
three M31 GCs for special reasons: S312 is among the first extragalactic GCs
whose age was estimated accurately using main-sequence photometry, while
037-B327 and G1 are among the most massive GCs in the Local Group. They have
been speculated to be nucleated dwarf galaxies instead of genuine GCs (see for
detailed discusions Ma et al., 2006c, 2007b). In this series of seven
articles, we published ages for 331 different M31 GCs and GC candidates.
Figure 5 show the age distribution of these 331 objects. We see that $\sim 40$
clusters are younger than 1 Gyr. The ages range from $<1$ to 20 Gyr (the upper
age limit in the BC96 and BC03 SSP models). A population of young clusters,
peaking at $\sim 3$ Gyr, is also apparent.

Figure 5.— Homogenized age distribution of the 331 M31 GCs and GC candidates
discussed in our series of papers.

Figure 6 shows the absolute magnitudes of our sample of M31 GCs and GC
candidates as a function of their age. The crosses indicate that the ages are
from Jiang et al. (2003), Ma et al. (2006a, b, 2007a, 2009a), and Fan et al.
(2006), which were obtained based on the SSP models of BC96 or BC03, while the
circles mean that the ages are from Ma et al. (2009a) and the present paper,
obtained on the basis of the galev SSP models. The dashed and solid lines
represent SSP models with $Z=0.004$ taken from BC03 and galev, respectively,
for masses of $10^{2}$, $10^{3}$, $10^{4}$, $10^{5}$, and $10^{6}M_{\odot}$
and assuming a Salpeter stellar IMF. The $V$-band photometry is from the RBC
v.3.5. The absolute magnitudes have been corrected for extinction (Barmby et
al., 2000; Fan et al., 2008), except for 037-B327, S312, and G1, the reddening
values of which are from Ma et al. (2006a), Ma et al. (2007a), and Ma et al.
(2009b), respectively. We adopt a distance modulus of $(m-M)_{0}=24.47$ mag
(McConnachie et al., 2005). Figure 6 shows that the majority of the clusters
have masses between $10^{3}$ and $10^{6}M_{\odot}$.

Figure 6.— Absolute $V$-band magnitudes for the M31 GCs and GC candidates as a
function of age. Overplotted are theoretical lines corresponding to (from
bottom to top) masses of $10^{2}$, $10^{3}$, $10^{4}$, $10^{5}$ and
$10^{6}M_{\odot}$ from BC03 (dashed line) and galev (solid line),
respectively.

The distribution of absolute $V$ magnitude of GCs in M31 is shown in Figure 7.
Overall, the distribution has a cutoff at the faint end with a magnitude limit
of about $-5.5$ mag (with a few fainter clusters still visible, probably
because of advantageous positions, e.g., observable through a hole in the
extinction distribution). The various cluster ages are separated in Figure 8,
which are: (i) very young ($t<1$ Gyr), (ii) young ($1\leq t<4$ Gyr), (iii)
intermediate-age ($4\leq t<10$ Gyr), and (iv) old GCs and GC candidates
($t\geq 10$ Gyr). We do not see a clear trend between age and brightness.
However, the youngest clusters are not the most massive objects, implying that
the conditions in the M31 have not been conducive to massive cluster formation
in the recent past.

Figure 7.— Histogram of the absolute $V$ magnitude for the 331 sample GCs and
GC candidates in M31.

Figure 8.— Histogram of the absolute $V$ magnitude for the M31 GCs and GC
candidates: (a) very young ($t<1$ Gyr), (b) young ($1\leq t<4$ Gyr), (c)
intermediate-age ($4\leq t<10$ Gyr), and (d) old GCs and GC candidates ($t\geq
10$ Gyr).

We converted the absolute magnitudes of our M31 GC sample to photometric
masses using the appropriate age-dependent mass-to-light ratios provided by
the BC03 and galev SSP models. The GC mass versus age diagram is shown in
Figure 9. The crosses indicate that the ages are from Jiang et al. (2003), Ma
et al. (2006a, b, 2007a, 2009a), and Fan et al. (2006), and the masses were
obtained based on the SSP models of BC03, while the circles mean that the ages
are from Ma et al. (2009a) and the present paper, and the masses were obtained
on the basis of the galev SSP models. Overplotted is the fading limit,
assuming $M_{V,{\rm limit}}=-5.5$ mag and evolutionary fading based on the
$Z=0.004$ BC03 (dashed line) and galev (solid line) models, assuming a
Salpeter stellar IMF. Figure 9 shows that our observational ($\sim 50$%)
completeness limit describes the lower mass limit of the entire GC sample up
to the oldest ages very well. Similarly, the upper envelope of the points in
Figure 9 is likely a result of the ‘size-of sample effect’ (e.g., Gieles &
Bastian, 2008, and references therein). It is clear, however, that massive
star cluster formation halted abruptly in the disk of M31 approximately 1 Gyr
ago. Given that massive ($>10^{4}M_{\odot}$) young ($<1$ Gyr-old) clusters
will be significantly brighter than the much older GC-type counterparts in
M31, we would have expected any such young massive clusters to have been
detected in M31, yet they have not.

Figure 9.— Distribution of the M31 GCs and GC candidates in the age-versus-
mass plane. Overplotted is the fading limit, based on the observed
$M_{V}=-5.5$ mag sample cutoff and the fading function from the cluster
evolutionary models with $Z=0.004$ taken from BC03 (dashed line) and galev
(solid line), assuming a Salpeter stellar IMF.

Using these 331 GCs and GC candidates with homogeneously determined ages, we
can now investigate their spatial distribution. We use an $X,Y$ projection to
refer to the relative positions of the objects. Our adopted $X$ coordinate
projects along M31’s major axis, where positive $X$ increases towards the
northeast, while the $Y$ coordinate extends along the minor axis of the M31
disk, increasing towards the northwest. To obtain the relative coordinates of
the M31 clusters, we adopted $\alpha_{0}=00^{\rm h}42^{\rm m}44^{\rm s}.30$
and $\delta_{0}=+41^{\circ}16^{\prime}09^{\prime\prime}.0$ (J2000.0) for M31’s
center, following Huchra et al. (1991) and Perrett et al. (2002). Formally,

$X=A\sin\theta+B\cos\theta\quad{\rm and}$ (6)

$Y=-A\cos\theta+B\sin\theta,$ (7)

where $A=\sin(\alpha-\alpha_{0})\cos\delta$ and
$B=\sin\delta\cos\delta_{0}-\cos(\alpha-\alpha_{0})\cos\delta\sin\delta_{0}$.
We adopt a position angle of $\theta=38^{\circ}$ for the major axis of M31
(Kent, 1989). We divided the GCs and GC candidates into four age groups: (i)
very young ($t<1$ Gyr), (ii) young ($1\leq t<4$ Gyr), (iii) intermediate-age
($4\leq t<10$ Gyr), and (iv) old GCs and GC candidates ($t\geq 10$ Gyr).
Figure 10 shows their spatial distributions. Although our sample of M31 GCs
and GC candidates is not complete (in spatial, radial terms, given that we are
limited by the six observed fields), we note that there is a tendency for
young GCs and GC candidates to be nearly uniformly distributed around M31. The
majority of old GCs appear to occupy the central regions of the galaxy,
although this restricted distribution may be caused by selection biases.
Figure 11 shows the number of GCs and GC candidates as a function of projected
radial distance from the M31 center, confirming our conclusions derived from
Figure 10. Figure 12 displays the cluster ages as a function of projected
radial distance. The crosses indicate that the ages are from Jiang et al.
(2003), Ma et al. (2006a, b, 2007a, 2009b), and Fan et al. (2006), which were
obtained using the BC96 or BC03 SSP models, while the circles indicate that
the ages are from Ma et al. (2009a) and the present paper, obtained on the
basis of the galev SSP models. Figure 12 shows that young GCs and GC
candidates are distributed nearly uniformly, and that most of the old GCs (and
candidates) are more concentrated.

Figure 10.— Spatial distribution of the M31 GCs and GC candidates: very young
($t<1$ Gyr), young ($1\leq t<4$ Gyr), intermediate-age ($4\leq t<10$ Gyr) and
old GCs and GC candidates ($t\geq 10$ Gyr).

Figure 11.— Radial distribution of the M31 GCs and GC candidates: (a) very
young ($t<1$ Gyr), (b) young ($1\leq t<4$ Gyr), (c) intermediate-age ($4\leq
t<10$ Gyr), and (d) old GCs and GC candidates ($t\geq 10$ Gyr).

Figure 12.— Age versus projected galactocentric radius for 331 M31 GCs and GC
candidates.

This paper presents photometry of 104 M31 globular clusters (GCs) and GC
candidates in 15 intermediate-band filters of the BATC photometric system. The
age of the clusters were obtained by comparing the photometric data with the
theoretical synthesis models. The ages of our sample clusters cover a large
range, although most clusters are younger than 10 Gyr. Combined with the ages
obtained in our series of previous papers focusing on the M31 GC system, we
present the full M31 GC age distribution. The results show that the M31 GC
system contains populations of young and intermediate-age GCs, as well as the
‘usual’ complement of well-known old GCs, i.e., GCs of similar age as the
majority of the Galactic GCs. In addition, young GCs (and GC candidates) are
distributed nearly uniformly in radial distance from the center of M31, while
most old GCs (and GC candidates) are more strongly concentrated.

We are indebted to the referee for thoughtful comments and insightful
suggestions that improved this paper significantly. This work was supported by
the Chinese National Natural Science Foundation (grants 10873016, 10633020,
10603006, and 10803007) and by National Basic Research Program of China (973
Program; grant 2007CB815403).

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Table 1BATC filter parameters Filter | Central wavelength | Bandwidth
---|---|---
| (Å) | (Å)
$a$ | 3360 | 360
$b$ | 3890 | 340
$c$ | 4210 | 320
$d$ | 4550 | 340
$e$ | 4925 | 390
$f$ | 5270 | 340
$g$ | 5795 | 310
$h$ | 6075 | 310
$i$ | 6660 | 480
$j$ | 7050 | 300
$k$ | 7490 | 330
$m$ | 8020 | 260
$n$ | 8480 | 180
$o$ | 9190 | 260
$p$ | 9745 | 270
Table 2BATC intermediate-band photometry (magnitudes) of 104 M31 GCs and GC candidates. Object | $a$ | $b$ | $c$ | $d$ | $e$ | $f$ | $g$ | $h$ | $i$ | $j$ | $k$ | $m$ | $n$ | $o$ | $p$
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
B001 | 19.08 | 18.94 | 18.32 | 17.68 | 17.49 | 17.23 | 16.78 | 16.65 | 16.37 | 16.28 | 16.10 | 15.89 | 15.89 | 15.72 | 15.67
| 0.190 | 0.045 | 0.022 | 0.038 | 0.032 | 0.016 | 0.021 | 0.011 | 0.008 | 0.013 | 0.012 | 0.011 | 0.016 | 0.021 | 0.019
B003 | … | 18.67 | 18.35 | 18.01 | 17.93 | 17.74 | 17.38 | 17.28 | 17.15 | 17.10 | 16.98 | 16.85 | 16.80 | 16.77 | 16.69
| … | 0.039 | 0.022 | 0.045 | 0.046 | 0.023 | 0.031 | 0.019 | 0.015 | 0.024 | 0.024 | 0.021 | 0.043 | 0.044 | 0.051
B005 | 18.07 | 17.23 | 16.66 | 16.01 | 15.94 | 15.78 | 15.43 | 15.32 | 15.08 | 15.05 | 14.90 | 14.86 | 14.86 | 14.68 | 14.62
| 0.037 | 0.019 | 0.017 | 0.016 | 0.012 | 0.010 | 0.010 | 0.008 | 0.006 | 0.007 | 0.009 | 0.007 | 0.008 | 0.011 | 0.013
B018 | 19.68 | 18.58 | 18.18 | 17.84 | 17.77 | 17.69 | 17.36 | 17.31 | 17.12 | 17.07 | 16.89 | 16.90 | 16.94 | 16.82 | 16.87
| 0.144 | 0.041 | 0.054 | 0.050 | 0.030 | 0.031 | 0.038 | 0.027 | 0.025 | 0.032 | 0.034 | 0.030 | 0.040 | 0.058 | 0.077
B020D | … | … | 18.43 | 18.09 | 17.80 | 17.52 | 17.16 | 17.09 | 16.85 | 16.68 | 16.55 | 16.40 | 16.37 | 16.13 | 16.12
| … | … | 0.056 | 0.044 | 0.037 | 0.033 | 0.027 | 0.024 | 0.023 | 0.021 | 0.022 | 0.018 | 0.033 | 0.024 | 0.037
B024 | … | 18.55 | 17.87 | 17.66 | 17.16 | 16.84 | 16.48 | 16.43 | 16.30 | 16.20 | 16.02 | 15.83 | 15.94 | 15.80 | 15.77
| … | 0.043 | 0.020 | 0.044 | 0.025 | 0.016 | 0.025 | 0.011 | 0.015 | 0.022 | 0.014 | 0.012 | 0.031 | 0.033 | 0.027
B046 | … | 19.23 | 18.66 | 18.36 | 18.21 | 17.85 | 17.39 | 17.45 | 17.29 | 17.15 | 17.02 | 16.81 | 17.03 | 17.20 | 16.70
| … | 0.076 | 0.034 | 0.097 | 0.085 | 0.036 | 0.053 | 0.028 | 0.076 | 0.086 | 0.039 | 0.035 | 0.081 | 0.104 | 0.070
B058 | 17.11 | 16.14 | 15.75 | 15.49 | 15.23 | 15.12 | 14.81 | 14.79 | 14.55 | 14.50 | 14.41 | 14.38 | 14.44 | 14.27 | 14.25
| 0.016 | 0.005 | 0.007 | 0.010 | 0.006 | 0.005 | 0.005 | 0.004 | 0.003 | 0.004 | 0.006 | 0.004 | 0.005 | 0.008 | 0.011
B083 | 19.10 | 18.73 | 17.97 | 17.90 | 17.32 | 17.03 | 16.70 | 16.63 | 16.55 | 16.43 | 16.20 | 15.98 | 16.20 | 16.09 | 15.91
| 0.138 | 0.045 | 0.020 | 0.084 | 0.039 | 0.021 | 0.031 | 0.015 | 0.026 | 0.037 | 0.017 | 0.014 | 0.044 | 0.046 | 0.041
B085 | 18.89 | 17.73 | 17.48 | 17.27 | 17.08 | 16.97 | 16.67 | 16.60 | 16.41 | 16.38 | 16.31 | 16.23 | 16.33 | 16.10 | 16.14
| 0.071 | 0.014 | 0.027 | 0.035 | 0.017 | 0.015 | 0.018 | 0.011 | 0.008 | 0.013 | 0.021 | 0.012 | 0.020 | 0.034 | 0.032
B138D | … | 18.51 | 18.39 | 17.61 | 17.04 | 16.84 | 16.48 | 16.38 | 16.16 | 16.07 | 15.94 | 15.70 | 15.69 | 15.66 | 15.47
| … | 0.050 | 0.021 | 0.035 | 0.023 | 0.012 | 0.015 | 0.009 | 0.007 | 0.012 | 0.010 | 0.010 | 0.013 | 0.019 | 0.018
B140D | … | 19.27 | 18.99 | 18.45 | 18.04 | 17.64 | 17.39 | 17.25 | 16.99 | 16.93 | 16.80 | 16.64 | 16.55 | 16.40 | 16.27
| … | 0.098 | 0.036 | 0.075 | 0.053 | 0.019 | 0.028 | 0.015 | 0.010 | 0.021 | 0.017 | 0.014 | 0.022 | 0.029 | 0.035
B141D | … | 19.22 | 18.76 | 18.22 | 17.87 | 17.33 | 17.12 | 16.91 | 16.67 | 16.65 | 16.52 | 16.32 | 16.18 | 16.09 | 16.03
| … | 0.096 | 0.030 | 0.063 | 0.046 | 0.015 | 0.022 | 0.012 | 0.008 | 0.017 | 0.015 | 0.012 | 0.018 | 0.024 | 0.028
B142D | 18.84 | 19.83 | 19.61 | 19.33 | 18.78 | 18.71 | 18.27 | 18.32 | 18.09 | 18.07 | 18.05 | 17.63 | 18.18 | 17.70 | 17.51
| 0.164 | 0.151 | 0.072 | 0.186 | 0.131 | 0.049 | 0.066 | 0.044 | 0.024 | 0.051 | 0.055 | 0.032 | 0.125 | 0.104 | 0.093
B144D | … | 19.93 | 19.05 | 18.25 | 18.04 | 18.06 | 17.55 | 17.42 | 17.20 | 17.10 | 16.95 | 16.79 | 16.84 | 16.70 | 16.67
| … | 0.176 | 0.041 | 0.060 | 0.050 | 0.025 | 0.032 | 0.017 | 0.012 | 0.024 | 0.019 | 0.017 | 0.034 | 0.038 | 0.048
B156D | … | 18.91 | 18.80 | 18.23 | 18.04 | 17.89 | 17.74 | 17.65 | 17.53 | 17.48 | 17.23 | 17.24 | 17.13 | 17.29 | 17.54
| … | 0.079 | 0.032 | 0.063 | 0.053 | 0.023 | 0.041 | 0.022 | 0.014 | 0.030 | 0.023 | 0.024 | 0.043 | 0.072 | 0.115
B157D | … | 19.62 | 19.23 | 18.46 | 18.06 | 17.78 | 17.40 | 17.32 | 17.13 | 17.06 | 16.91 | 16.66 | 16.70 | 16.58 | 16.47
| … | 0.107 | 0.044 | 0.067 | 0.053 | 0.020 | 0.030 | 0.017 | 0.011 | 0.021 | 0.019 | 0.015 | 0.029 | 0.044 | 0.035
B165D | … | 19.14 | 18.79 | 18.17 | 17.97 | 17.78 | 17.60 | 17.48 | 17.28 | 17.07 | 17.10 | 16.87 | 16.79 | 16.90 | 16.64
| … | 0.061 | 0.030 | 0.061 | 0.045 | 0.021 | 0.033 | 0.016 | 0.012 | 0.020 | 0.022 | 0.018 | 0.029 | 0.058 | 0.037
B166D | … | 19.53 | 19.43 | 18.33 | 18.33 | 18.18 | 17.73 | 17.62 | 17.41 | 17.30 | 17.18 | 17.03 | 17.00 | 16.97 | 17.07
| … | 0.055 | 0.147 | 0.065 | 0.037 | 0.039 | 0.038 | 0.022 | 0.012 | 0.020 | 0.035 | 0.020 | 0.029 | 0.052 | 0.089
B167D | … | 19.07 | 18.55 | 18.33 | 18.26 | 17.89 | 17.56 | 17.52 | 17.43 | 17.38 | 17.31 | 17.09 | 17.15 | 17.05 | 17.11
| … | 0.051 | 0.031 | 0.084 | 0.086 | 0.030 | 0.054 | 0.023 | 0.036 | 0.050 | 0.034 | 0.027 | 0.058 | 0.103 | 0.092
B172D | 19.55 | 18.76 | 18.52 | 17.82 | 18.11 | 18.10 | 17.92 | 17.89 | 17.82 | 17.89 | 17.97 | 17.79 | 17.99 | 18.05 | 17.89
| 0.094 | 0.043 | 0.063 | 0.048 | 0.033 | 0.035 | 0.045 | 0.025 | 0.025 | 0.044 | 0.078 | 0.043 | 0.112 | 0.160 | 0.134
B177D | 20.11 | 19.37 | 18.97 | 18.50 | 18.40 | 18.34 | 18.09 | 17.98 | 17.78 | 17.87 | 17.74 | 17.81 | 18.04 | 17.76 | 17.75
| 0.158 | 0.062 | 0.095 | 0.074 | 0.045 | 0.041 | 0.051 | 0.028 | 0.021 | 0.034 | 0.055 | 0.040 | 0.074 | 0.099 | 0.143
B181D | … | 19.12 | 18.64 | 18.19 | 17.94 | 17.85 | 17.65 | 17.51 | 17.38 | 17.30 | 17.26 | 17.16 | 17.25 | 17.34 | 17.03
| … | 0.074 | 0.028 | 0.055 | 0.038 | 0.023 | 0.036 | 0.017 | 0.017 | 0.026 | 0.025 | 0.030 | 0.054 | 0.057 | 0.062
B196 | … | 18.43 | 18.15 | 17.77 | 17.58 | 17.40 | 17.16 | 17.05 | 16.79 | 16.74 | 16.64 | 16.65 | 16.62 | 16.58 | 16.60
| … | 0.071 | 0.021 | 0.027 | 0.025 | 0.022 | 0.039 | 0.021 | 0.011 | 0.034 | 0.020 | 0.015 | 0.037 | 0.048 | 0.035
B223D | … | … | 19.31 | 18.64 | 18.10 | 17.94 | 17.39 | 17.29 | 17.03 | 16.94 | 16.70 | 16.60 | 16.48 | 16.44 | 16.20
| … | … | 0.132 | 0.069 | 0.044 | 0.083 | 0.040 | 0.019 | 0.009 | 0.020 | 0.027 | 0.016 | 0.024 | 0.035 | 0.045
B240 | 17.13 | 16.39 | 15.93 | 15.69 | 15.50 | 15.35 | 15.11 | 15.00 | 14.85 | 14.78 | 14.68 | 14.59 | 14.61 | 14.56 | 14.48
| 0.035 | 0.009 | 0.004 | 0.009 | 0.006 | 0.005 | 0.006 | 0.003 | 0.003 | 0.005 | 0.005 | 0.004 | 0.007 | 0.006 | 0.017
B244 | … | 19.00 | 18.95 | 18.36 | 18.43 | 18.38 | 17.97 | 17.98 | 17.82 | 17.72 | 17.63 | 17.55 | 17.46 | 17.52 | 17.40
| … | 0.058 | 0.043 | 0.067 | 0.066 | 0.037 | 0.054 | 0.033 | 0.028 | 0.037 | 0.039 | 0.032 | 0.071 | 0.077 | 0.092
B245D | … | 19.86 | 19.27 | 18.69 | 18.60 | 18.36 | 18.00 | 18.14 | 18.00 | 17.88 | 17.88 | 17.74 | 17.88 | 18.01 | 18.11
| … | 0.177 | 0.135 | 0.083 | 0.083 | 0.131 | 0.081 | 0.054 | 0.040 | 0.058 | 0.076 | 0.061 | 0.089 | 0.169 | 0.251
B257 | … | … | 19.32 | 18.62 | 18.34 | 17.99 | 17.50 | 17.35 | 16.99 | 16.83 | 16.62 | 16.52 | 16.40 | 16.16 | 16.11
| … | … | 0.085 | 0.056 | 0.056 | 0.049 | 0.042 | 0.037 | 0.032 | 0.032 | 0.033 | 0.029 | 0.043 | 0.032 | 0.039
B260 | … | … | 20.51 | 19.76 | 19.53 | 18.95 | 18.25 | 18.06 | 17.57 | 17.35 | 17.02 | 16.82 | 16.62 | 16.27 | 16.12
| … | … | 0.399 | 0.235 | 0.226 | 0.147 | 0.105 | 0.087 | 0.066 | 0.058 | 0.050 | 0.043 | 0.058 | 0.035 | 0.036
B261D | 19.10 | 18.32 | 18.10 | 17.82 | 17.65 | 17.45 | 17.28 | 17.34 | 17.27 | 17.17 | 17.09 | 16.93 | 17.09 | 16.98 | 17.32
| 0.120 | 0.034 | 0.047 | 0.026 | 0.035 | 0.062 | 0.041 | 0.022 | 0.013 | 0.026 | 0.039 | 0.023 | 0.042 | 0.048 | 0.115
Table 2Continued. Object | $a$ | $b$ | $c$ | $d$ | $e$ | $f$ | $g$ | $h$ | $i$ | $j$ | $k$ | $m$ | $n$ | $o$ | $p$
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
B266 | … | … | 20.00 | 19.47 | 18.86 | 18.67 | 18.05 | 17.93 | 17.63 | 17.49 | 17.30 | 17.14 | 17.02 | 16.91 | 16.83
| … | … | 0.150 | 0.103 | 0.065 | 0.056 | 0.042 | 0.037 | 0.029 | 0.031 | 0.030 | 0.031 | 0.052 | 0.038 | 0.059
B270D | … | 18.62 | 18.25 | 18.05 | 17.84 | 17.62 | 17.42 | 17.27 | 17.15 | 17.05 | 16.98 | 16.92 | 16.87 | 16.93 | 16.83
| … | 0.052 | 0.020 | 0.043 | 0.026 | 0.019 | 0.030 | 0.012 | 0.012 | 0.018 | 0.019 | 0.017 | 0.031 | 0.033 | 0.129
B272 | … | … | 19.75 | 19.01 | 18.61 | 18.39 | 17.91 | 17.82 | 17.58 | 17.40 | 17.16 | 17.02 | 16.95 | 16.74 | 16.56
| … | … | 0.084 | 0.054 | 0.039 | 0.031 | 0.033 | 0.028 | 0.026 | 0.026 | 0.035 | 0.027 | 0.056 | 0.034 | 0.046
B281 | … | … | 18.62 | 18.23 | 17.99 | 17.80 | 17.53 | 17.42 | 17.23 | 17.16 | 17.00 | 16.90 | 16.90 | 16.67 | 16.67
| … | … | 0.034 | 0.025 | 0.022 | 0.025 | 0.024 | 0.024 | 0.025 | 0.026 | 0.030 | 0.027 | 0.042 | 0.034 | 0.057
B283D | 18.97 | 18.39 | 18.07 | 17.82 | 17.58 | 17.59 | 17.30 | 17.29 | 17.15 | 17.14 | 17.00 | 16.86 | 16.92 | 16.73 | 16.79
| 0.105 | 0.037 | 0.042 | 0.030 | 0.033 | 0.058 | 0.036 | 0.024 | 0.014 | 0.026 | 0.031 | 0.022 | 0.041 | 0.046 | 0.071
B283 | … | 19.45 | 18.66 | 18.42 | 18.03 | 17.89 | 17.55 | 17.47 | 17.27 | 17.18 | 17.04 | 16.93 | 17.07 | 16.78 | 16.80
| … | 0.132 | 0.034 | 0.062 | 0.036 | 0.030 | 0.040 | 0.023 | 0.021 | 0.027 | 0.031 | 0.025 | 0.071 | 0.028 | 0.134
B289D | 19.63 | 19.33 | 19.07 | 18.62 | 18.51 | 18.75 | 18.02 | 18.04 | 17.96 | 17.95 | 17.71 | 17.62 | 17.72 | 17.62 | 17.47
| 0.180 | 0.068 | 0.100 | 0.053 | 0.076 | 0.169 | 0.077 | 0.039 | 0.025 | 0.053 | 0.071 | 0.042 | 0.083 | 0.078 | 0.142
B292D | … | 19.06 | 19.01 | 18.34 | 18.00 | 17.91 | 17.62 | 17.51 | 17.38 | 17.37 | 17.33 | 17.05 | 17.04 | 17.12 | 16.85
| … | 0.055 | 0.102 | 0.041 | 0.047 | 0.092 | 0.050 | 0.028 | 0.016 | 0.032 | 0.047 | 0.025 | 0.044 | 0.052 | 0.077
B292 | 19.01 | 18.18 | 17.81 | 17.43 | 17.29 | 17.22 | 16.96 | 16.90 | 16.76 | 16.70 | 16.70 | 16.54 | 16.58 | 16.43 | 16.46
| 0.183 | 0.026 | 0.014 | 0.034 | 0.030 | 0.015 | 0.019 | 0.012 | 0.008 | 0.016 | 0.016 | 0.013 | 0.022 | 0.031 | 0.030
B293D | 19.58 | 18.58 | 18.36 | 18.08 | 18.14 | 17.79 | 17.76 | 17.60 | 17.59 | 17.50 | 17.36 | 17.32 | 17.38 | 17.08 | 17.32
| 0.186 | 0.065 | 0.022 | 0.034 | 0.047 | 0.040 | 0.065 | 0.033 | 0.024 | 0.036 | 0.041 | 0.033 | 0.135 | 0.076 | 0.099
B297D | … | … | 19.46 | 18.64 | 18.11 | 17.77 | 17.26 | 17.14 | 16.85 | 16.75 | 16.48 | 16.16 | 16.15 | 16.12 | 15.77
| … | … | 0.149 | 0.049 | 0.051 | 0.080 | 0.040 | 0.019 | 0.010 | 0.017 | 0.024 | 0.013 | 0.022 | 0.025 | 0.030
B301 | 19.56 | 18.62 | 18.14 | 17.36 | 17.40 | 17.28 | 16.96 | 16.85 | 16.60 | 16.57 | 16.52 | 16.44 | 16.41 | 16.34 | 16.18
| 0.093 | 0.028 | 0.043 | 0.030 | 0.020 | 0.018 | 0.022 | 0.013 | 0.008 | 0.013 | 0.021 | 0.015 | 0.019 | 0.029 | 0.041
B303 | 19.52 | 18.62 | 18.26 | 17.96 | 18.06 | 18.00 | 18.04 | 17.88 | 17.84 | 18.24 | 18.56 | 18.18 | 18.41 | 18.28 | 18.10
| 0.104 | 0.033 | 0.053 | 0.055 | 0.032 | 0.035 | 0.057 | 0.034 | 0.029 | 0.074 | 0.166 | 0.072 | 0.117 | 0.211 | 0.244
B304 | 18.92 | 17.84 | 17.53 | 17.19 | 17.13 | 16.93 | 16.65 | 16.58 | 16.43 | 16.40 | 16.34 | 16.19 | 16.19 | 16.14 | 16.14
| 0.189 | 0.021 | 0.011 | 0.025 | 0.030 | 0.013 | 0.017 | 0.010 | 0.007 | 0.013 | 0.013 | 0.011 | 0.022 | 0.028 | 0.030
B305 | 19.89 | 19.06 | 18.67 | 17.98 | 18.11 | 18.03 | 17.74 | 17.61 | 17.51 | 17.53 | 17.45 | 17.44 | 17.46 | 17.29 | 16.94
| 0.120 | 0.054 | 0.076 | 0.059 | 0.031 | 0.034 | 0.041 | 0.026 | 0.017 | 0.027 | 0.054 | 0.034 | 0.049 | 0.066 | 0.080
B306 | 19.47 | 18.17 | 17.69 | 16.71 | 16.78 | 16.54 | 16.07 | 15.88 | 15.57 | 15.48 | 15.29 | 15.17 | 15.15 | 14.91 | 14.79
| 0.113 | 0.023 | 0.033 | 0.020 | 0.013 | 0.011 | 0.011 | 0.008 | 0.004 | 0.006 | 0.008 | 0.006 | 0.007 | 0.010 | 0.015
B307 | 19.79 | 18.52 | 18.12 | 17.58 | 17.59 | 17.51 | 17.26 | 17.17 | 16.97 | 16.97 | 16.74 | 16.74 | 16.85 | 16.58 | 16.46
| 0.152 | 0.033 | 0.051 | 0.038 | 0.023 | 0.021 | 0.028 | 0.018 | 0.012 | 0.019 | 0.029 | 0.019 | 0.030 | 0.039 | 0.054
B309 | 19.98 | 18.78 | 18.55 | 17.80 | 17.88 | 17.75 | 17.44 | 17.31 | 17.12 | 17.10 | 17.15 | 17.03 | 17.04 | 17.01 | 17.05
| 0.148 | 0.054 | 0.077 | 0.054 | 0.033 | 0.034 | 0.037 | 0.021 | 0.020 | 0.028 | 0.056 | 0.035 | 0.044 | 0.088 | 0.118
B310 | 18.99 | 18.05 | 17.77 | 17.45 | 17.32 | 17.16 | 16.85 | 16.76 | 16.63 | 16.57 | 16.50 | 16.35 | 16.33 | 16.27 | 16.24
| 0.153 | 0.027 | 0.014 | 0.031 | 0.025 | 0.014 | 0.019 | 0.010 | 0.009 | 0.015 | 0.016 | 0.014 | 0.024 | 0.027 | 0.033
B311 | 17.64 | 16.62 | 16.33 | 15.81 | 15.79 | 15.61 | 15.32 | 15.20 | 14.98 | 14.95 | 14.83 | 14.79 | 14.79 | 14.63 | 14.61
| 0.024 | 0.007 | 0.011 | 0.012 | 0.007 | 0.006 | 0.007 | 0.005 | 0.003 | 0.005 | 0.008 | 0.005 | 0.007 | 0.010 | 0.011
B312 | 18.04 | 16.91 | 16.47 | 16.01 | 15.86 | 15.68 | 15.28 | 15.22 | 15.01 | 14.94 | 14.82 | 14.65 | 14.67 | 14.59 | 14.53
| 0.082 | 0.009 | 0.006 | 0.012 | 0.010 | 0.006 | 0.007 | 0.005 | 0.003 | 0.006 | 0.005 | 0.005 | 0.007 | 0.010 | 0.009
B313 | 18.85 | 17.99 | 17.47 | 16.82 | 16.74 | 16.57 | 16.17 | 16.08 | 15.82 | 15.76 | 15.58 | 15.49 | 15.47 | 15.24 | 15.22
| 0.063 | 0.026 | 0.034 | 0.024 | 0.016 | 0.012 | 0.013 | 0.009 | 0.006 | 0.009 | 0.011 | 0.008 | 0.012 | 0.014 | 0.018
B315 | 17.56 | 16.63 | 16.51 | 16.20 | 16.42 | 16.38 | 16.23 | 16.23 | 16.10 | 16.13 | 16.08 | 16.09 | 16.18 | 16.03 | 15.93
| 0.024 | 0.008 | 0.013 | 0.016 | 0.012 | 0.013 | 0.014 | 0.012 | 0.010 | 0.013 | 0.018 | 0.015 | 0.025 | 0.028 | 0.034
B316 | … | 18.28 | 17.75 | 17.25 | 17.24 | 17.21 | 16.95 | 16.82 | 16.67 | 16.65 | 16.55 | 16.57 | 16.60 | 16.48 | 16.42
| … | 0.028 | 0.038 | 0.030 | 0.020 | 0.021 | 0.025 | 0.018 | 0.014 | 0.019 | 0.025 | 0.019 | 0.027 | 0.038 | 0.049
B317 | 18.66 | 17.67 | 17.28 | 17.37 | 16.93 | 16.65 | 16.37 | 16.33 | 16.29 | 16.21 | 16.12 | 15.94 | 16.02 | 15.93 | 15.98
| 0.097 | 0.019 | 0.014 | 0.044 | 0.022 | 0.013 | 0.023 | 0.012 | 0.017 | 0.021 | 0.015 | 0.012 | 0.021 | 0.025 | 0.038
B325 | 18.50 | 17.81 | 17.55 | 17.12 | 17.27 | 17.19 | 16.92 | 16.86 | 16.70 | 16.71 | 16.64 | 16.63 | 16.69 | 16.42 | 16.55
| 0.053 | 0.027 | 0.034 | 0.036 | 0.026 | 0.023 | 0.024 | 0.017 | 0.014 | 0.019 | 0.034 | 0.019 | 0.030 | 0.050 | 0.053
B332D | … | … | 18.87 | 18.46 | 17.85 | 17.34 | 17.10 | 16.88 | 16.66 | 16.56 | 16.32 | 16.27 | 16.16 | 16.03 | 16.02
| … | … | 0.036 | 0.064 | 0.027 | 0.015 | 0.023 | 0.010 | 0.008 | 0.014 | 0.016 | 0.013 | 0.021 | 0.014 | 0.067
B335 | … | 19.60 | 19.15 | 18.77 | 18.36 | 18.15 | 17.64 | 17.49 | 17.12 | 17.07 | 16.76 | 16.71 | 16.69 | 16.52 | 16.23
| … | 0.101 | 0.132 | 0.116 | 0.053 | 0.050 | 0.047 | 0.033 | 0.024 | 0.031 | 0.040 | 0.024 | 0.029 | 0.051 | 0.046
B337 | 18.77 | 17.85 | 17.51 | 17.43 | 17.04 | 16.76 | 16.43 | 16.35 | 16.32 | 16.20 | 16.09 | 15.89 | 16.01 | 15.93 | 15.89
| 0.100 | 0.027 | 0.015 | 0.046 | 0.021 | 0.014 | 0.021 | 0.010 | 0.012 | 0.028 | 0.013 | 0.011 | 0.018 | 0.031 | 0.031
B338 | 16.31 | 15.36 | 15.02 | 14.59 | 14.53 | 14.41 | 14.11 | 14.05 | 13.84 | 13.82 | 13.71 | 13.71 | 13.73 | 13.57 | 13.54
| 0.011 | 0.005 | 0.005 | 0.006 | 0.004 | 0.003 | 0.004 | 0.003 | 0.002 | 0.003 | 0.004 | 0.003 | 0.003 | 0.005 | 0.008
B340D | … | … | 19.39 | 19.59 | 18.15 | 18.64 | 17.79 | 17.58 | 17.23 | 17.31 | 16.93 | 16.83 | 16.74 | 16.66 | 16.76
| … | … | 0.135 | 0.644 | 0.144 | 0.304 | 0.062 | 0.025 | 0.020 | 0.056 | 0.026 | 0.024 | 0.055 | 0.030 | 0.107
Table 2Continued. Object | $a$ | $b$ | $c$ | $d$ | $e$ | $f$ | $g$ | $h$ | $i$ | $j$ | $k$ | $m$ | $n$ | $o$ | $p$
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
B343 | 18.22 | 17.19 | 16.94 | 16.53 | 16.55 | 16.48 | 16.20 | 16.11 | 15.91 | 15.92 | 15.79 | 15.80 | 15.84 | 15.74 | 15.72
| 0.039 | 0.012 | 0.016 | 0.019 | 0.012 | 0.010 | 0.012 | 0.008 | 0.005 | 0.009 | 0.012 | 0.008 | 0.013 | 0.017 | 0.028
B344 | 18.17 | 17.32 | 16.79 | 16.62 | 16.22 | 15.96 | 15.59 | 15.49 | 15.40 | 15.32 | 15.16 | 14.98 | 15.07 | 14.95 | 14.93
| 0.063 | 0.015 | 0.009 | 0.018 | 0.015 | 0.008 | 0.012 | 0.006 | 0.006 | 0.010 | 0.007 | 0.006 | 0.008 | 0.015 | 0.015
B347 | 18.35 | 17.54 | 17.13 | 17.15 | 16.71 | 16.51 | 16.17 | 16.09 | 16.03 | 15.94 | 15.84 | 15.63 | 15.75 | 15.60 | 15.71
| 0.064 | 0.017 | 0.011 | 0.026 | 0.023 | 0.012 | 0.018 | 0.009 | 0.011 | 0.016 | 0.011 | 0.010 | 0.020 | 0.030 | 0.028
B348 | 19.28 | 18.49 | 17.86 | 17.63 | 17.18 | 16.84 | 16.47 | 16.48 | 16.36 | 16.26 | 16.08 | 15.89 | 15.98 | 15.83 | 15.84
| 0.172 | 0.042 | 0.024 | 0.054 | 0.036 | 0.018 | 0.030 | 0.014 | 0.020 | 0.023 | 0.017 | 0.013 | 0.027 | 0.039 | 0.033
B350 | 18.61 | 17.61 | 17.28 | 16.84 | 16.91 | 16.89 | 16.51 | 16.48 | 16.25 | 16.23 | 16.10 | 16.10 | 16.15 | 15.95 | 16.00
| 0.049 | 0.013 | 0.022 | 0.024 | 0.015 | 0.013 | 0.015 | 0.010 | 0.006 | 0.010 | 0.016 | 0.009 | 0.017 | 0.021 | 0.034
B351 | 19.34 | 18.70 | 18.33 | 18.12 | 17.84 | 17.93 | 17.36 | 17.11 | 17.14 | 17.13 | 17.04 | 16.78 | 16.85 | 16.77 | 16.77
| 0.134 | 0.053 | 0.055 | 0.040 | 0.036 | 0.102 | 0.039 | 0.019 | 0.011 | 0.023 | 0.032 | 0.018 | 0.030 | 0.051 | 0.066
B352 | 18.59 | 17.61 | 17.18 | 17.01 | 16.81 | 16.59 | 16.32 | 16.31 | 16.14 | 16.08 | 16.02 | 15.83 | 15.89 | 15.86 | 15.79
| 0.070 | 0.022 | 0.020 | 0.018 | 0.016 | 0.032 | 0.017 | 0.010 | 0.005 | 0.011 | 0.014 | 0.010 | 0.015 | 0.024 | 0.029
B354 | 19.34 | 18.86 | 18.52 | 18.31 | 18.02 | 18.08 | 17.49 | 17.52 | 17.38 | 17.34 | 17.27 | 17.06 | 17.11 | 16.96 | 16.92
| 0.139 | 0.065 | 0.065 | 0.060 | 0.039 | 0.099 | 0.042 | 0.026 | 0.014 | 0.030 | 0.041 | 0.022 | 0.042 | 0.056 | 0.073
B356 | 19.34 | 18.31 | 17.85 | 17.59 | 17.32 | 17.08 | 16.77 | 16.71 | 16.47 | 16.41 | 16.30 | 16.07 | 16.15 | 16.00 | 16.00
| 0.146 | 0.046 | 0.036 | 0.034 | 0.025 | 0.044 | 0.026 | 0.015 | 0.008 | 0.015 | 0.018 | 0.014 | 0.018 | 0.031 | 0.034
B357 | 18.84 | 18.02 | 17.52 | 17.00 | 16.86 | 16.68 | 16.47 | 16.33 | 16.12 | 16.02 | 15.92 | 15.94 | 15.88 | 15.75 | 15.74
| 0.094 | 0.041 | 0.012 | 0.014 | 0.014 | 0.013 | 0.022 | 0.011 | 0.005 | 0.014 | 0.012 | 0.009 | 0.023 | 0.024 | 0.023
B361 | 18.91 | 17.88 | 17.67 | 17.32 | 17.23 | 17.12 | 16.95 | 16.82 | 16.63 | 16.63 | 16.53 | 16.58 | 16.48 | 16.49 | 16.42
| 0.089 | 0.034 | 0.014 | 0.017 | 0.019 | 0.017 | 0.029 | 0.017 | 0.007 | 0.023 | 0.017 | 0.012 | 0.029 | 0.047 | 0.033
B365 | 18.77 | 17.75 | 17.44 | 17.24 | 16.93 | 16.76 | 16.52 | 16.45 | 16.29 | 16.26 | 16.04 | 15.92 | 15.97 | 15.95 | 15.88
| 0.088 | 0.023 | 0.027 | 0.019 | 0.019 | 0.035 | 0.021 | 0.012 | 0.006 | 0.012 | 0.022 | 0.011 | 0.018 | 0.023 | 0.034
B370 | 18.23 | 17.43 | 17.11 | 16.84 | 16.52 | 16.31 | 16.00 | 15.95 | 15.73 | 15.67 | 15.52 | 15.33 | 15.39 | 15.29 | 15.20
| 0.052 | 0.020 | 0.021 | 0.016 | 0.018 | 0.027 | 0.016 | 0.011 | 0.007 | 0.010 | 0.012 | 0.009 | 0.012 | 0.016 | 0.021
B372 | 18.82 | 17.71 | 17.43 | 17.07 | 16.81 | 16.69 | 16.36 | 16.30 | 16.10 | 16.09 | 15.91 | 15.76 | 15.82 | 15.77 | 15.69
| 0.095 | 0.024 | 0.026 | 0.020 | 0.020 | 0.033 | 0.020 | 0.012 | 0.007 | 0.011 | 0.015 | 0.011 | 0.016 | 0.023 | 0.027
B373 | 18.06 | 17.37 | 16.73 | 16.27 | 15.94 | 15.75 | 15.40 | 15.37 | 15.13 | 15.06 | 14.84 | 14.67 | 14.72 | 14.58 | 14.48
| 0.049 | 0.018 | 0.015 | 0.010 | 0.011 | 0.018 | 0.009 | 0.007 | 0.004 | 0.006 | 0.007 | 0.006 | 0.008 | 0.010 | 0.013
B375 | … | 18.92 | 18.51 | 18.34 | 17.92 | 17.73 | 17.38 | 17.32 | 17.13 | 17.02 | 16.87 | 16.78 | 16.85 | 16.66 | 16.48
| … | 0.068 | 0.033 | 0.061 | 0.037 | 0.026 | 0.035 | 0.022 | 0.020 | 0.026 | 0.031 | 0.028 | 0.043 | 0.041 | 0.106
B377 | 19.28 | 18.08 | 17.70 | 17.45 | 17.34 | 17.16 | 17.03 | 16.82 | 16.67 | 16.67 | 16.56 | 16.63 | 16.54 | 16.49 | 16.47
| 0.127 | 0.049 | 0.014 | 0.019 | 0.023 | 0.017 | 0.033 | 0.019 | 0.009 | 0.023 | 0.021 | 0.013 | 0.036 | 0.042 | 0.041
B378 | … | 18.49 | 18.38 | 18.18 | 17.80 | 17.65 | 17.36 | 17.42 | 17.23 | 17.17 | 17.05 | 16.91 | 17.09 | 16.97 | 17.05
| … | 0.044 | 0.059 | 0.047 | 0.043 | 0.070 | 0.045 | 0.036 | 0.021 | 0.036 | 0.044 | 0.032 | 0.052 | 0.071 | 0.092
B382 | … | 18.51 | 18.01 | 17.87 | 17.59 | 17.42 | 17.19 | 17.10 | 16.96 | 16.89 | 16.77 | 16.66 | 16.71 | 16.70 | 16.80
| … | 0.050 | 0.021 | 0.037 | 0.026 | 0.019 | 0.027 | 0.013 | 0.015 | 0.021 | 0.029 | 0.022 | 0.040 | 0.039 | 0.121
B383 | 18.06 | 17.30 | 16.72 | 16.30 | 16.05 | 15.88 | 15.57 | 15.43 | 15.24 | 15.16 | 14.96 | 14.87 | 14.87 | 14.75 | 14.72
| 0.088 | 0.017 | 0.007 | 0.013 | 0.009 | 0.007 | 0.008 | 0.004 | 0.004 | 0.006 | 0.006 | 0.005 | 0.008 | 0.007 | 0.020
B384 | 18.14 | 17.18 | 16.78 | 16.34 | 16.17 | 16.02 | 15.69 | 15.57 | 15.34 | 15.26 | 15.10 | 15.12 | 15.16 | 14.97 | 14.97
| 0.046 | 0.018 | 0.007 | 0.009 | 0.012 | 0.008 | 0.012 | 0.007 | 0.003 | 0.008 | 0.007 | 0.005 | 0.010 | 0.011 | 0.011
B386 | 17.75 | 16.84 | 16.48 | 16.17 | 15.86 | 15.70 | 15.38 | 15.35 | 15.14 | 15.11 | 14.97 | 14.79 | 14.84 | 14.79 | 14.71
| 0.035 | 0.009 | 0.012 | 0.008 | 0.009 | 0.017 | 0.009 | 0.006 | 0.003 | 0.005 | 0.008 | 0.005 | 0.008 | 0.011 | 0.014
B387 | 19.14 | 17.73 | 17.63 | 17.47 | 17.30 | 17.14 | 16.97 | 16.85 | 16.66 | 16.65 | 16.54 | 16.55 | 16.65 | 16.44 | 16.32
| 0.106 | 0.037 | 0.013 | 0.021 | 0.023 | 0.017 | 0.032 | 0.015 | 0.010 | 0.020 | 0.021 | 0.013 | 0.035 | 0.046 | 0.029
B393 | … | 18.25 | 17.83 | 17.54 | 17.26 | 17.09 | 16.80 | 16.69 | 16.53 | 16.49 | 16.33 | 16.25 | 16.21 | 16.14 | 16.03
| … | 0.039 | 0.016 | 0.029 | 0.018 | 0.014 | 0.019 | 0.009 | 0.008 | 0.013 | 0.013 | 0.011 | 0.026 | 0.015 | 0.046
B399 | … | 18.38 | 18.05 | 18.01 | 17.58 | 17.45 | 17.23 | 17.14 | 17.03 | 16.92 | 16.82 | 16.79 | 16.91 | 16.78 | 16.90
| … | 0.049 | 0.019 | 0.044 | 0.025 | 0.018 | 0.028 | 0.013 | 0.011 | 0.019 | 0.024 | 0.018 | 0.047 | 0.029 | 0.134
B401 | 18.67 | 17.70 | 17.39 | 17.43 | 17.07 | 16.92 | 16.69 | 16.59 | 16.47 | 16.42 | 16.29 | 16.20 | 16.23 | 16.20 | 16.22
| 0.149 | 0.030 | 0.012 | 0.029 | 0.017 | 0.013 | 0.020 | 0.010 | 0.009 | 0.014 | 0.014 | 0.013 | 0.023 | 0.019 | 0.085
B403 | 18.77 | 17.75 | 17.20 | 17.07 | 16.54 | 16.40 | 16.06 | 15.93 | 15.75 | 15.66 | 15.47 | 15.35 | 15.39 | 15.27 | 15.29
| 0.133 | 0.032 | 0.009 | 0.023 | 0.012 | 0.009 | 0.011 | 0.006 | 0.005 | 0.008 | 0.009 | 0.007 | 0.013 | 0.009 | 0.030
B405 | 17.33 | 16.26 | 15.85 | 15.87 | 15.43 | 15.29 | 15.01 | 14.90 | 14.74 | 14.69 | 14.52 | 14.43 | 14.47 | 14.41 | 14.42
| 0.043 | 0.010 | 0.004 | 0.010 | 0.006 | 0.005 | 0.005 | 0.003 | 0.003 | 0.005 | 0.005 | 0.004 | 0.006 | 0.005 | 0.018
B420 | … | 19.36 | 19.18 | 18.45 | 17.91 | 17.67 | 17.36 | 17.20 | 16.98 | 16.90 | 16.79 | 16.56 | 16.50 | 16.48 | 16.20
| … | 0.110 | 0.046 | 0.073 | 0.039 | 0.020 | 0.030 | 0.015 | 0.011 | 0.021 | 0.018 | 0.015 | 0.026 | 0.035 | 0.032
B448 | 19.60 | 18.24 | 18.15 | 17.92 | 17.95 | 17.89 | 17.59 | 17.58 | 17.44 | 17.40 | 17.45 | 17.38 | 17.40 | 17.44 | 17.18
| 0.136 | 0.037 | 0.060 | 0.067 | 0.052 | 0.058 | 0.055 | 0.050 | 0.048 | 0.054 | 0.069 | 0.059 | 0.071 | 0.121 | 0.088
B457 | 19.20 | 18.25 | 17.91 | 17.90 | 17.48 | 17.21 | 16.91 | 16.84 | 16.76 | 16.66 | 16.55 | 16.35 | 16.42 | 16.44 | 16.43
| 0.139 | 0.041 | 0.020 | 0.072 | 0.034 | 0.021 | 0.035 | 0.015 | 0.023 | 0.039 | 0.019 | 0.017 | 0.045 | 0.061 | 0.051
Table 2Continued. Object | $a$ | $b$ | $c$ | $d$ | $e$ | $f$ | $g$ | $h$ | $i$ | $j$ | $k$ | $m$ | $n$ | $o$ | $p$
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
B461 | 19.41 | 18.91 | 18.38 | 18.15 | 17.67 | 17.49 | 17.09 | 16.99 | 16.85 | 16.78 | 16.62 | 16.41 | 16.54 | 16.39 | 16.43
| 0.157 | 0.056 | 0.027 | 0.067 | 0.047 | 0.020 | 0.036 | 0.016 | 0.018 | 0.034 | 0.017 | 0.014 | 0.026 | 0.050 | 0.054
B462 | … | 19.03 | 18.77 | 18.67 | 18.42 | 18.19 | 17.80 | 17.74 | 17.66 | 17.52 | 17.45 | 17.30 | 17.44 | 17.29 | 17.37
| … | 0.063 | 0.040 | 0.112 | 0.092 | 0.036 | 0.065 | 0.030 | 0.036 | 0.061 | 0.032 | 0.027 | 0.058 | 0.090 | 0.130
B467 | … | 18.57 | 18.25 | 18.00 | 17.83 | 17.51 | 17.35 | 17.25 | 17.11 | 17.02 | 17.08 | 16.82 | 16.86 | 16.75 | 16.84
| … | 0.052 | 0.052 | 0.044 | 0.035 | 0.060 | 0.039 | 0.021 | 0.012 | 0.024 | 0.038 | 0.019 | 0.032 | 0.046 | 0.063
B472 | 17.60 | 16.43 | 16.00 | 15.68 | 15.40 | 15.25 | 14.95 | 14.89 | 14.75 | 14.66 | 14.58 | 14.46 | 14.40 | 14.35 | 14.35
| 0.025 | 0.024 | 0.009 | 0.007 | 0.006 | 0.006 | 0.006 | 0.006 | 0.006 | 0.006 | 0.007 | 0.006 | 0.009 | 0.008 | 0.012
B475 | 19.38 | 18.08 | 17.74 | 17.66 | 17.50 | 17.36 | 17.28 | 17.37 | 17.21 | 17.17 | 17.00 | 16.97 | 16.95 | 16.71 | 16.57
| 0.156 | 0.047 | 0.050 | 0.054 | 0.062 | 0.074 | 0.066 | 0.069 | 0.053 | 0.061 | 0.076 | 0.061 | 0.067 | 0.068 | 0.071
B476 | … | … | 19.26 | 18.87 | 18.72 | 18.50 | 18.14 | 18.12 | 17.95 | 17.87 | 17.70 | 17.49 | 17.68 | 17.46 | 17.68
| … | … | 0.064 | 0.093 | 0.076 | 0.050 | 0.068 | 0.037 | 0.037 | 0.053 | 0.070 | 0.054 | 0.096 | 0.083 | 0.254
B483 | … | 18.86 | 18.62 | 18.49 | 18.32 | 18.17 | 18.33 | 18.11 | 18.13 | 18.20 | 18.11 | 17.86 | 18.03 | 18.07 | 17.58
| … | 0.059 | 0.071 | 0.054 | 0.062 | 0.103 | 0.096 | 0.044 | 0.039 | 0.069 | 0.095 | 0.055 | 0.099 | 0.130 | 0.146
B486 | … | 18.68 | 18.19 | 18.03 | 17.83 | 17.65 | 17.48 | 17.40 | 17.23 | 17.15 | 17.11 | 17.05 | 17.03 | 16.89 | 16.86
| … | 0.055 | 0.019 | 0.042 | 0.027 | 0.019 | 0.031 | 0.014 | 0.014 | 0.023 | 0.021 | 0.020 | 0.058 | 0.036 | 0.123
B489 | … | 19.32 | 18.88 | 18.01 | 17.65 | 17.33 | 17.12 | 16.91 | 16.70 | 16.57 | 16.40 | 16.32 | 16.26 | 16.15 | 15.98
| … | 0.112 | 0.033 | 0.035 | 0.036 | 0.030 | 0.041 | 0.020 | 0.010 | 0.021 | 0.022 | 0.013 | 0.052 | 0.034 | 0.035
B495 | … | … | 19.59 | 18.82 | 18.16 | 17.95 | 17.38 | 17.19 | 16.94 | 16.85 | 16.58 | 16.34 | 16.26 | 16.22 | 15.93
| … | … | 0.160 | 0.075 | 0.046 | 0.077 | 0.039 | 0.020 | 0.009 | 0.019 | 0.020 | 0.013 | 0.021 | 0.028 | 0.034
G260 | 19.07 | 18.05 | 17.75 | 17.57 | 17.22 | 17.11 | 16.79 | 16.74 | 16.62 | 16.58 | 16.45 | 16.25 | 16.29 | 16.28 | 16.26
| 0.112 | 0.027 | 0.034 | 0.025 | 0.023 | 0.041 | 0.025 | 0.013 | 0.007 | 0.015 | 0.023 | 0.013 | 0.023 | 0.031 | 0.047
Table 3GALEX, optical broad-band, and 2MASS NIR photometry of 104 M31 GCs and
GC candidates.

Object |  $c$† | FUV | NUV | $U$ | $B$ | $V$ | $R$ | $I$ | $J$ | $H$ | $K_{\rm s}$
---|---|---|---|---|---|---|---|---|---|---|---
B001 | 1 | … | … | 18.82 | 18.33 | 17.06 | 16.47 | 15.41 | 14.69 | 13.73 | 13.84
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.04 | 0.05
B003 | 1 | 23.06 | 21.55 | 18.40 | 18.35 | 17.57 | 17.07 | 16.41 | 15.95 | 15.15 | 15.51
|  | 0.20 | 0.04 | 0.04 | 0.02 | 0.01 | 0.03 | 0.02 | 0.08 | 0.10 | 0.12
B005 | 1 | … | 21.08 | 16.12 | 16.04 | 15.44 | 14.99 | 14.66 | 13.40 | 12.69 | 12.51
|  | … | 0.12 | 0.02 | 0.01 | 0.01 | 0.01 | 0.01 | 0.03 | 0.03 | 0.03
B018 | 1 | … | 22.09 | 18.47 | 18.25 | 17.53 | 17.00 | 16.38 | 15.47 | 14.77 | 14.59
|  | … | 0.15 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B020D | 1 | … | … | 18.99 | 18.43 | 17.44 | … | 16.04 | 14.91 | 14.62 | 13.98
|  | … | … | 0.08 | 0.05 | 0.05 | … | 0.05 | 0.04 | 0.07 | 0.05
B024 | 1 | … | 22.51 | 18.40 | 17.75 | 16.80 | 16.27 | 15.65 | 14.80 | 14.25 | 13.98
|  | … | 0.07 | 0.08 | 0.02 | 0.01 | 0.01 | 0.01 | 0.04 | 0.07 | 0.05
B046 | 1 | 22.80 | 21.71 | 18.70 | 18.65 | 17.81 | 17.37 | 16.87 | 15.91 | 14.83 | 14.93
|  | 0.16 | 0.05 | 0.09 | 0.03 | 0.01 | 0.04 | 0.03 | 0.08 | 0.07 | 0.10
B058 | 1 | 20.23 | 19.09 | 16.05 | 15.81 | 15.01 | 14.48 | 13.91 | 13.13 | 12.50 | 12.36
|  | 0.04 | 0.01 | 0.01 | 0.01 | 0.01 | 0.01 | 0.01 | 0.03 | 0.03 | 0.03
B083 | 1 | 22.60 | 21.45 | 17.91 | 17.85 | 17.09 | 16.55 | 15.93 | 15.32 | 14.61 | 14.59
|  | 0.14 | 0.03 | 0.04 | 0.02 | 0.01 | 0.02 | 0.01 | 0.08 | 0.07 | 0.10
B085 | 1 | 22.24 | 20.60 | 17.92 | 17.55 | 16.84 | 16.38 | 15.63 | 15.03 | 14.72 | 14.29
|  | 0.11 | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B138D | 2 | 23.11 | 22.38 | 18.70 | 17.92 | 16.87 | 16.14 | … | 14.24 | 13.48 | 13.18
|  | 0.18 | 0.06 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.04 | 0.04 | 0.05
B140D | 2 | 22.31 | 21.73 | 18.74 | 18.87 | 17.67 | 17.04 | … | 15.17 | 14.45 | 13.99
|  | 0.08 | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.07 | 0.05
B141D | 2 | … | … | 18.89 | 18.73 | 17.43 | 16.69 | … | 14.75 | 14.04 | 13.55
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.04 | 0.07 | 0.05
B142D | 2 | 21.21 | 21.21 | 19.06 | 19.80 | 18.63 | 17.93 | … | 16.99 | … | 14.98
|  | 0.10 | 0.07 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.10 | … | 0.10
B144D | 2 | … | … | 19.37 | 18.85 | 17.72 | 17.06 | … | 15.70 | 15.02 | 14.96
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.10 | 0.10
B156D | 2 | 20.97 | 20.29 | 18.57 | 18.88 | 18.16 | 17.49 | … | 16.15 | … | 15.18
|  | 0.04 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.10 | … | 0.12
B157D | 2 | … | … | 19.37 | 19.06 | 17.83 | 17.24 | … | 15.19 | 14.62 | 14.03
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.07 | 0.10
B165D | 2 | 21.06 | 20.82 | 18.92 | 18.68 | 17.62 | 17.34 | … | 15.63 | 14.72 | 14.19
|  | 0.06 | 0.04 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.07 | 0.10
B166D | 2 | … | … | 19.11 | 18.90 | 17.93 | 17.34 | … | 15.47 | 14.83 | 14.41
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.07 | 0.10
B167D | 1 | 22.09 | 21.34 | 18.41 | 18.54 | 17.79 | 17.31 | … | 16.36 | 15.65 | 15.28
|  | 0.07 | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.10 | 0.10 | 0.12
B172D | 2 | … | 21.71 | 18.44 | 18.64 | 17.97 | 17.61 | … | … | … | …
|  | … | 0.08 | 0.08 | 0.05 | 0.05 | 0.05 | … | … | … | …
B177D | 2 | … | … | 19.11 | 18.89 | 18.09 | 17.63 | … | … | … | …
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | … | … | …
B181D | 2 | … | … | 18.73 | 18.71 | 17.72 | 17.14 | … | 15.24 | 16.41 | …
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.10 | …
B196 | 1 | … | 21.60 | 18.35 | 18.05 | 17.40 | 16.75 | 16.10 | 15.54 | 14.57 | 14.82
|  | … | 0.10 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B223D | 2 | … | 22.86 | 19.30 | 18.74 | 17.75 | … | … | 15.25 | 14.19 | 13.81
|  | … | 0.13 | 0.08 | 0.05 | 0.05 | … | … | 0.08 | 0.07 | 0.05
B240 | 1 | 19.90 | 18.94 | 16.03 | 15.93 | 15.23 | 14.73 | 14.20 | 13.47 | 12.90 | 12.76
|  | 0.04 | 0.01 | 0.01 | 0.01 | 0.01 | 0.01 | 0.01 | 0.03 | 0.03 | 0.03
B244 | 2 | … | 22.23 | 19.13 | 19.05 | 18.27 | 17.66 | 17.22 | 15.46 | 15.36 | …
|  | … | 0.07 | 0.08 | 0.04 | 0.01 | 0.05 | 0.04 | 0.08 | 0.10 | …
B245D | 2 | … | … | 18.91 | 19.08 | 18.22 | 17.56 | … | 16.20 | 16.65 | …
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.10 | 0.10 | …
B257 | 2 | … | … | 19.75 | 19.43 | 20.96 | … | 16.31 | 14.79 | 13.98 | 13.69
|  | … | … | 0.08 | 0.05 | 0.05 | … | 0.05 | 0.04 | 0.04 | 0.05
B260 | 2 | … | … | … | … | 18.50 | 17.52 | 16.42 | 14.69 | 13.90 | 13.74
|  | … | … | … | … | 0.01 | 0.01 | 0.07 | 0.04 | 0.04 | 0.05

††footnotetext: New classification flag (RBC v.3.5): 1 = GC, 2 = candidate GC.

Table 3Continued.

Object |  $c$† | FUV | NUV | $U$ | $B$ | $V$ | $R$ | $I$ | $J$ | $H$ | $K_{\rm s}$
---|---|---|---|---|---|---|---|---|---|---|---
B261D | 2 | … | 21.31 | 18.02 | 18.06 | 17.60 | 16.97 | … | 15.35 | 15.38 | …
|  | … | 0.04 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.10 | …
B266 | 1 | … | … | 18.76 | 19.29 | 18.32 | 17.40 | 16.50 | 15.64 | 15.06 | 14.45
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.10
B270D | 2 | … | 21.81 | 18.24 | 17.90 | 17.50 | 16.94 | … | 15.43 | 15.09 | …
|  | … | 0.07 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.10 | …
B272 | 1 | … | … | 19.94 | 19.52 | 18.20 | 17.50 | 16.61 | 14.70 | 14.40 | …
|  | … | … | 0.08 | 0.06 | 0.01 | 0.05 | 0.05 | 0.04 | 0.07 | …
B281 | 1 | … | … | 19.01 | 18.51 | 17.67 | 17.11 | 16.51 | 15.87 | 14.88 | 14.26
|  | … | … | 0.06 | 0.03 | 0.01 | 0.03 | 0.03 | 0.08 | 0.07 | 0.10
B283D | 2 | … | 21.02 | 18.11 | 18.12 | 17.51 | 16.97 | … | 15.16 | 14.87 | …
|  | … | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.07 | …
B283 | 1 | … | … | 19.63 | 18.70 | 17.64 | 17.20 | 16.53 | 15.73 | 14.90 | 15.05
|  | … | … | 0.08 | 0.04 | 0.01 | 0.03 | 0.02 | 0.08 | 0.07 | 0.12
B289D | 1 | … | … | 18.94 | 18.94 | 18.09 | 17.74 | … | 15.49 | … | …
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | … | …
B292D | 1 | … | … | 18.95 | 18.89 | 17.81 | … | … | 15.39 | 15.25 | …
|  | … | … | 0.08 | 0.05 | 0.05 | … | … | 0.08 | 0.10 | …
B292 | 1 | 21.80 | 21.02 | 17.87 | 17.89 | 17.00 | 16.62 | 16.06 | 15.41 | 15.03 | 14.71
|  | 0.09 | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.10
B293D | 2 | … | 21.32 | 18.33 | 18.45 | 17.91 | 17.29 | … | 16.52 | 15.99 | 15.41
|  | … | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.10 | 0.10 | 0.12
B297D | 2 | … | … | 20.06 | 19.05 | 17.63 | … | … | 14.66 | 13.90 | 13.70
|  | … | … | 0.08 | 0.05 | 0.05 | … | … | 0.04 | 0.04 | 0.05
B301 | 1 | … | … | 18.48 | 18.13 | 17.12 | 16.53 | 15.71 | 15.08 | 14.31 | 14.06
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B303 | 1 | … | 21.15 | 18.92 | 18.46 | 18.22 | 17.50 | 17.03 | … | … | …
|  | … | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | … | … | …
B304 | 1 | 22.03 | 20.69 | 17.78 | 17.54 | 16.83 | 16.32 | 15.74 | 15.12 | 14.46 | 14.27
|  | 0.08 | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B305 | 1 | … | 22.69 | 18.68 | 18.82 | 17.93 | 17.21 | 17.00 | 15.80 | 15.48 | 15.34
|  | … | 0.18 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.12
B306 | 1 | … | 22.31 | 18.19 | 17.55 | 16.30 | 15.59 | 14.63 | 13.55 | 12.74 | 12.58
|  | … | 0.15 | 0.08 | 0.05 | 0.01 | 0.05 | 0.01 | 0.03 | 0.03 | 0.03
B307 | 1 | … | 21.84 | 19.20 | 18.19 | 17.32 | 17.15 | 16.10 | 15.22 | 14.56 | 14.18
|  | … | 0.08 | 0.08 | 0.05 | 0.01 | 0.05 | 0.01 | 0.08 | 0.07 | 0.10
B309 | 1 | … | 22.00 | 18.63 | 18.47 | 17.50 | 17.00 | 15.80 | 16.01 | … | 15.92
|  | … | 0.10 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.10 | … | 0.12
B310 | 1 | 22.03 | 20.87 | 18.03 | 17.80 | 17.04 | 16.54 | 15.98 | 15.24 | 14.65 | 14.63
|  | 0.08 | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B311 | 1 | 21.18 | 19.72 | 16.55 | 16.41 | 15.44 | 14.94 | 14.22 | 13.50 | 12.86 | 12.70
|  | 0.06 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.03 | 0.03 | 0.03
B312 | 1 | 21.06 | 20.08 | 16.68 | 16.34 | 15.52 | 14.96 | 14.16 | 13.56 | 12.85 | 12.78
|  | 0.10 | 0.04 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.03 | 0.03 | 0.03
B313 | 1 | … | 20.77 | 18.11 | 17.41 | 16.37 | 15.79 | 14.96 | 14.06 | 13.30 | 13.11
|  | … | 0.12 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.04 | 0.05
B315 | 1 | 18.70 | 18.36 | 16.57 | 16.55 | 16.47 | 16.03 | 15.58 | 14.82 | 14.67 | 13.98
|  | 0.02 | 0.01 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.07 | 0.05
B316 | 1 | … | … | 18.10 | 17.77 | 17.06 | 16.39 | 16.14 | 14.71 | 14.43 | …
|  | … | … | 0.08 | 0.02 | 0.01 | 0.02 | 0.02 | 0.04 | 0.07 | …
B317 | 1 | 21.67 | 20.27 | 17.58 | 17.30 | 16.57 | 16.13 | 15.71 | 14.98 | 14.53 | 14.50
|  | 0.05 | 0.01 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.07 | 0.10
B325 | 1 | 19.93 | … | … | 17.54 | 16.94 | 16.42 | 15.91 | 15.22 | 14.57 | 14.38
|  | 0.06 | … | … | 0.02 | 0.01 | 0.02 | 0.02 | 0.08 | 0.07 | 0.10
B332D | 2 | … | … | 19.02 | 18.70 | 17.21 | 16.60 | … | 14.81 | 13.86 | 13.55
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.04 | 0.04 | 0.05
B335 | 1 | … | … | 19.99 | 19.04 | 17.89 | 16.91 | 16.14 | 14.94 | 14.24 | 13.94
|  | … | … | 0.08 | 0.06 | 0.01 | 0.04 | 0.03 | 0.04 | 0.07 | 0.05
B337 | 1 | 21.89 | 20.70 | 17.69 | 17.52 | 16.73 | 16.24 | 15.63 | 15.06 | 14.47 | 14.06
|  | 0.06 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10

††footnotetext: New classification flag (RBC v.3.5): 1 = GC, 2 = candidate GC.

Table 3Continued.

Object |  $c$† | FUV | NUV | $U$ | $B$ | $V$ | $R$ | $I$ | $J$ | $H$ | $K_{\rm s}$
---|---|---|---|---|---|---|---|---|---|---|---
B338 | 1 | 19.05 | 18.28 | 15.21 | 15.06 | 14.30 | 13.67 | 13.28 | 12.45 | 11.79 | 11.67
|  | 0.02 | 0.01 | 0.01 | 0.01 | 0.01 | 0.05 | 0.01 | 0.02 | 0.02 | 0.02
B340D | 2 | … | … | 20.22 | 19.93 | 17.92 | 17.22 | … | 15.53 | 14.55 | 14.45
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.07 | 0.10
B343 | 1 | 20.80 | 19.90 | 17.23 | 17.08 | 16.31 | 15.91 | 15.27 | 14.63 | 13.94 | 13.90
|  | 0.06 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.04 | 0.05
B344 | 1 | … | 20.75 | 17.01 | 16.77 | 15.95 | 15.33 | 14.87 | 14.02 | 13.40 | 13.35
|  | … | 0.02 | 0.08 | 0.05 | 0.01 | 0.05 | 0.01 | 0.04 | 0.04 | 0.05
B347 | 1 | 22.10 | 20.26 | 17.38 | 17.23 | 16.50 | 15.97 | 15.49 | 14.75 | 14.04 | 14.11
|  | 0.08 | 0.02 | 0.08 | 0.05 | 0.01 | 0.05 | 0.01 | 0.04 | 0.07 | 0.10
B348 | 1 | … | 22.06 | 18.33 | 17.98 | 16.79 | 16.33 | 15.64 | 14.78 | 14.34 | 13.93
|  | … | 0.07 | 0.08 | 0.05 | 0.01 | 0.05 | 0.01 | 0.04 | 0.07 | 0.05
B350 | 1 | 21.77 | 20.47 | 17.47 | 17.36 | 16.74 | 16.20 | 15.64 | 14.84 | 14.46 | 14.19
|  | 0.08 | 0.03 | 0.08 | 0.05 | 0.01 | 0.05 | 0.01 | 0.04 | 0.07 | 0.10
B351 | 1 | … | 21.67 | 18.61 | 18.40 | 17.55 | 17.07 | 16.43 | 15.98 | 15.22 | 14.88
|  | … | 0.04 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.10
B352 | 1 | 21.11 | 20.08 | 17.42 | 17.25 | 16.54 | 15.96 | 15.57 | 14.93 | 14.28 | 14.11
|  | 0.05 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.07 | 0.10
B354 | 1 | … | 21.69 | 18.63 | 17.94 | 17.81 | 17.19 | 16.74 | 16.01 | 15.21 | 15.25
|  | … | 0.05 | 0.08 | 0.05 | 0.01 | 0.05 | 0.02 | 0.10 | 0.10 | 0.12
B356 | 1 | 22.33 | 21.43 | 18.42 | 18.12 | 17.34 | 16.43 | 15.71 | 14.93 | 14.29 | 14.24
|  | 0.17 | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.07 | 0.10
B357 | 1 | … | 21.81 | 17.98 | 17.49 | 16.61 | 15.97 | 15.39 | 14.48 | 13.80 | 13.68
|  | … | 0.07 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.04 | 0.05
B361 | 1 | 21.40 | 20.54 | 17.92 | 17.78 | 17.05 | 16.57 | 16.01 | 15.32 | 14.71 | 14.56
|  | 0.07 | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B365 | 1 | 21.64 | 20.58 | 17.72 | 17.51 | 16.72 | 15.90 | 15.57 | 14.97 | 14.24 | 14.10
|  | 0.05 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.07 | 0.10
B370 | 1 | 21.48 | 20.53 | 17.28 | 17.15 | 16.30 | 15.63 | 15.14 | 14.17 | 13.44 | 13.34
|  | 0.05 | 0.02 | 0.03 | 0.01 | 0.01 | 0.01 | 0.01 | 0.04 | 0.04 | 0.05
B372 | 1 | … | 20.97 | 17.71 | 17.48 | 16.60 | 15.84 | 15.50 | 14.68 | 13.95 | 13.80
|  | … | 0.04 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.04 | 0.05
B373 | 1 | … | 21.23 | 17.07 | 16.58 | 15.64 | 15.13 | 14.39 | 13.36 | 12.57 | 12.46
|  | … | 0.07 | 0.03 | 0.01 | 0.01 | 0.01 | 0.01 | 0.03 | 0.03 | 0.03
B375 | 1 | … | 22.44 | 19.87 | 18.51 | 17.61 | 17.07 | 16.59 | 15.49 | 14.68 | 14.32
|  | … | 0.19 | 0.08 | 0.03 | 0.01 | 0.03 | 0.04 | 0.08 | 0.07 | 0.10
B377 | 1 | … | 20.70 | 17.83 | 17.77 | 17.14 | 16.64 | 16.20 | 15.43 | 15.09 | 14.44
|  | … | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.10
B378 | 1 | … | 21.49 | 18.85 | 18.52 | 17.83 | 16.94 | 16.50 | 15.99 | 15.40 | 15.19
|  | … | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.12
B382 | 1 | 21.91 | 20.97 | 18.28 | 18.15 | 17.36 | 16.74 | 16.08 | 15.69 | 15.09 | 15.52
|  | 0.10 | 0.04 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.12
B383 | 1 | … | 21.21 | 17.23 | 16.17 | 15.33 | 14.87 | 14.43 | 13.58 | 12.85 | 12.66
|  | … | 0.06 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.03 | 0.03 | 0.03
B384 | 1 | … | 21.32 | 17.37 | 16.74 | 15.75 | 15.26 | 14.56 | 13.76 | 13.01 | 12.91
|  | … | 0.07 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.03 | 0.04 | 0.03
B386 | 1 | 21.64 | 20.00 | 16.68 | 16.45 | 15.55 | 14.75 | 14.39 | 13.70 | 12.95 | 12.83
|  | 0.08 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.03 | 0.03 | 0.03
B387 | 1 | … | 20.69 | 17.84 | 17.66 | 16.98 | 16.48 | 16.05 | 15.32 | 14.94 | 14.43
|  | … | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B393 | 1 | … | 21.75 | 17.97 | 17.72 | 16.93 | 16.40 | 16.00 | 15.18 | 14.23 | 14.21
|  | … | 0.09 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B399 | 1 | … | 21.00 | 18.25 | 18.05 | 17.28 | 16.85 | 16.23 | 15.80 | 15.50 | 15.35
|  | … | 0.08 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.12
B401 | 1 | … | 20.43 | 17.83 | 17.51 | 16.83 | 16.50 | 15.68 | 15.09 | 14.60 | 14.56
|  | … | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B403 | 1 | … | 21.59 | 17.62 | 17.19 | 16.22 | 15.68 | 15.00 | 14.15 | 13.48 | 13.24
|  | … | 0.11 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.04 | 0.05
B405 | 1 | 19.72 | 18.89 | 16.22 | 15.93 | 15.19 | 14.66 | … | 13.41 | 12.77 | 12.66
|  | 0.06 | 0.02 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.03 | 0.03 | 0.03

††footnotetext: New classification flag (RBC v.3.5): 1 = GC, 2 = candidate GC.

Table 3Continued.

Object |  $c$† | FUV | NUV | $U$ | $B$ | $V$ | $R$ | $I$ | $J$ | $H$ | $K_{\rm s}$
---|---|---|---|---|---|---|---|---|---|---|---
B420 | 2 | … | … | 19.68 | 18.96 | 17.85 | 17.12 | 16.13 | 15.16 | 14.68 | 14.15
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B448 | 1 | 21.90 | 21.14 | 18.11 | 18.10 | 17.49 | 17.06 | 16.77 | … | … | …
|  | 0.12 | 0.05 | 0.09 | 0.04 | 0.01 | 0.04 | 0.03 | … | … | …
B457 | 1 | … | 21.21 | 18.05 | 17.73 | 16.91 | 16.38 | 16.87 | 14.68 | 14.78 | …
|  | … | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.07 | …
B461 | 1 | … | 22.82 | 18.73 | 18.77 | 17.52 | 16.89 | 16.04 | 15.55 | 14.67 | 14.61
|  | … | 0.14 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.07 | 0.10
B462 | 1 | … | 21.96 | 18.82 | 18.83 | 18.06 | 17.38 | 17.01 | 15.45 | … | …
|  | … | 0.06 | 0.08 | 0.05 | 0.01 | 0.05 | 0.02 | 0.08 | … | …
B467 | 1 | 22.49 | 21.33 | 18.36 | 18.31 | 17.43 | 16.85 | 16.15 | 15.96 | 15.73 | 15.18
|  | 0.10 | 0.03 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.12
B472 | 1 | 19.93 | 19.03 | 16.16 | 15.97 | 15.19 | 14.67 | 14.12 | 13.34 | 12.69 | 12.60
|  | 0.04 | 0.02 | 0.01 | 0.01 | 0.01 | 0.01 | 0.01 | 0.03 | 0.03 | 0.03
B475 | 1 | … | 21.07 | 17.97 | 17.87 | 17.56 | 17.03 | 16.91 | 16.04 | 15.01 | 14.63
|  | … | 0.06 | 0.10 | 0.03 | 0.01 | 0.04 | 0.04 | 0.10 | 0.10 | 0.10
B476 | 2 | … | … | 19.52 | 19.12 | 18.12 | 17.69 | 17.00 | 15.34 | 14.68 | …
|  | … | … | 0.09 | 0.05 | 0.01 | 0.06 | 0.05 | 0.08 | 0.07 | …
B483 | 1 | … | 21.73 | 18.81 | 18.73 | 18.46 | 17.75 | 17.82 | … | … | …
|  | … | 0.05 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | … | … | …
B486 | 1 | … | 21.36 | 18.80 | 17.87 | 17.52 | 17.03 | 16.49 | 15.90 | 15.54 | 15.46
|  | … | 0.09 | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.08 | 0.10 | 0.12
B489 | 2 | … | … | 19.32 | 18.47 | 17.35 | 16.66 | 15.64 | 14.76 | 13.99 | 13.80
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.04 | 0.05
B495 | 2 | … | … | 19.60 | 19.02 | 17.61 | 17.04 | 15.82 | 14.83 | 14.02 | 13.74
|  | … | … | 0.08 | 0.05 | 0.05 | 0.05 | 0.05 | 0.04 | 0.07 | 0.05
G260 | 1 | 22.69 | 21.11 | 17.64 | 17.81 | 17.01 | 16.53 | … | 15.25 | 14.80 | 14.59
|  | 0.13 | 0.04 | 0.08 | 0.05 | 0.05 | 0.05 | … | 0.08 | 0.07 | 0.10

††footnotetext: New classification flag (RBC v.3.5): 1 = GC, 2 = candidate GC.

Table 4Reddening values (magnitudes) and metallicities (dex) for 104 M31 GCs
and GC candidates.

Object | $E(B-V)$ | ref.a | $\rm[Fe/H]$ | ref.b
---|---|---|---|---
B001 | 0.25$\pm$ 0.02 | 1 |  $-0.58\pm$ 0.18 | 1
B003 | 0.19$\pm$ 0.02 | 1 |  $-2.08\pm$ 0.07 | 4
B005 | 0.28$\pm$ 0.02 | 1 |  $-1.18\pm$ 0.17 | 1
B018 | 0.20$\pm$ 0.01 | 1 |  $-1.63\pm$ 0.77 | 1
B020D | 0.22$\pm$ 0.06 | 1 |  $-0.76\pm$ 0.08 | 4
B024 | 0.03$\pm$ 0.02 | 1 |  $-0.48\pm$ 0.30 | 3
B046 | 0.19$\pm$ 0.03 | 1 |  $-1.84\pm$ 0.61 | 3
B058 | 0.13$\pm$ 0.01 | 1 |  $-1.45\pm$ 0.24 | 3
B083 | 0.12$\pm$ 0.02 | 1 |  $-1.18\pm$ 0.44 | 1
B085 | 0.14$\pm$ 0.02 | 1 |  $-1.83\pm$ 0.40 | 3
B138D | 0.23$\pm$ 0.04 | 1 |  $-0.36\pm$ 0.04 | 4
B140D | 0.45$\pm$ 0.11 | 1 |  $-1.57\pm$ 0.12 | 4
B141D | 0.43$\pm$ 0.09 | 1 |  $-1.07\pm$ 0.08 | 4
B142D | 0.58$\pm$ 0.03 | 1 |  $-2.59\pm$ 0.24 | 4
B144D | 0.33$\pm$ 0.02 | 1 |  $-1.62\pm$ 0.09 | 4
B156D | 0.45$\pm$ 0.09 | 1 |  $-2.58\pm$ 0.14 | 4
B157D | 0.15$\pm$ 0.01 | 1 |  $-0.09\pm$ 0.08 | 4
B165D | 0.21$\pm$ 0.07 | 1 |  $-1.05\pm$ 0.13 | 4
B166D | 0.26$\pm$ 0.04 | 1 |  $-1.02\pm$ 0.08 | 4
B167D | 0.23$\pm$ 0.03 | 1 |  $-2.34\pm$ 0.08 | 4
B172D | 0.11$\pm$ 0.05 | 1 |  $-2.51\pm$ 0.12 | 4
B177D | 0.08$\pm$ 0.02 | 1 |  $-1.32\pm$ 0.01 | 4
B181D | 0.36$\pm$ 0.09 | 1 |  $-2.21\pm$ 0.20 | 4
B196 | 0.26$\pm$ 0.04 | 1 |  $-1.94\pm$ 0.08 | 4
B223D | 0.20$\pm$ 0.05 | 1 |  $-0.23\pm$ 0.08 | 4
B240 | 0.13$\pm$ 0.00 | 1 |  $-1.76\pm$ 0.18 | 3
B244 | 0.27$\pm$ 0.03 | 1 |  $-1.50\pm$ 0.21 | 4
B245D | 0.52$\pm$ 0.03 | 1 |  $-2.88\pm$ 0.09 | 4
B257 | 1.17$\pm$ 0.03 | 1 |  $-2.05\pm$ 0.82 | 4
B260 | 0.67$\pm$ 0.02 | 1 |  $-0.36\pm$ 0.10 | 4
B261D | 0.27$\pm$ 0.06 | 1 |  $-2.45\pm$ 0.19 | 4
B266 | 0.98$\pm$ 0.09 | 1 |  $-2.80\pm$ 0.15 | 4
B270D | 0.25$\pm$ 0.02 | 1 |  $-2.28\pm$ 0.19 | 4
B272 | 0.57$\pm$ 0.04 | 1 |  $-1.25\pm$ 0.16 | 1
B281 | 0.12$\pm$ 0.02 | 1 |  $-0.87\pm$ 0.52 | 1
B283D | 0.16$\pm$ 0.04 | 1 |  $-1.55\pm$ 0.17 | 4
B283 | 0.08$\pm$ 0.06 | 2 |  $-0.06\pm$ 0.20 | 1
B289D | 0.23$\pm$ 0.05 | 1 |  $-1.71\pm$ 0.63 | 1
B292D | 0.23$\pm$ 0.14 | 2 |  $-0.47\pm$ 0.54 | 1
B292 | 0.23$\pm$ 0.14 | 2 |  $-1.42\pm$ 0.16 | 2
B293D | 0.27$\pm$ 0.06 | 1 |  $-2.57\pm$ 0.11 | 4
B297D | 0.30$\pm$ 0.07 | 1 |  $0.10\pm$ 0.08 | 4
B301 | 0.17$\pm$ 0.02 | 1 |  $-0.76\pm$ 0.25 | 1
B303 | 0.14$\pm$ 0.06 | 1 |  $-2.09\pm$ 0.41 | 1
B304 | 0.07$\pm$ 0.01 | 1 |  $-1.32\pm$ 0.22 | 2
B305 | 0.38$\pm$ 0.29 | 2 |  $-0.90\pm$ 0.61 | 1
B306 | 0.42$\pm$ 0.02 | 1 |  $-0.85\pm$ 0.71 | 1
B307 | 0.08$\pm$ 0.02 | 1 |  $-0.41\pm$ 0.36 | 1
B309 | 0.17$\pm$ 0.04 | 1 |  $-2.03\pm$ 0.26 | 4
B310 | 0.09$\pm$ 0.01 | 1 |  $-1.43\pm$ 0.28 | 2
B311 | 0.29$\pm$ 0.02 | 1 |  $-1.96\pm$ 0.07 | 1
B312 | 0.16$\pm$ 0.01 | 1 |  $-1.41\pm$ 0.08 | 1

aafootnotetext: The reddening values are taken from Fan et al. (2008) (ref=1)
and Barmby et al. (2000) (ref=2).

bbfootnotetext: The metallicities are taken from Perrett et al. (2002)
(ref=1), Barmby et al. (2000) (ref=2), Huchra et al. (1991) (ref=3), and Fan
et al. (2008) (ref=4).

Table 4Continuted.

Object | $E(B-V)$ | ref.a | $\rm[Fe/H]$ | ref.b
---|---|---|---|---
B313 | 0.21$\pm$ 0.02 | 1 |  $-1.09\pm$ 0.10 | 1
B315 | 0.07$\pm$ 0.02 | 1 |  $-2.35\pm$ 0.54 | 1
B316 | 0.21$\pm$ 0.03 | 1 |  $-1.47\pm$ 0.23 | 1
B317 | 0.11$\pm$ 0.02 | 1 |  $-2.12\pm$ 0.36 | 3
B325 | 0.14$\pm$ 0.02 | 1 |  $-1.77\pm$ 0.08 | 4
B332D | 0.33$\pm$ 0.13 | 1 |  $-0.65\pm$ 0.09 | 4
B335 | 0.65$\pm$ 0.02 | 1 |  $-1.05\pm$ 0.26 | 1
B337 | 0.06$\pm$ 0.02 | 1 |  $-1.09\pm$ 0.32 | 2
B338 | 0.14$\pm$ 0.02 | 1 |  $-1.46\pm$ 0.12 | 1
B340D | 0.23$\pm$ 0.06 | 1 |  $0.19\pm$ 0.29 | 4
B343 | 0.06$\pm$ 0.01 | 1 |  $-1.49\pm$ 0.17 | 3
B344 | 0.11$\pm$ 0.02 | 1 |  $-1.13\pm$ 0.21 | 3
B347 | 0.14$\pm$ 0.02 | 1 |  $-1.71\pm$ 0.03 | 4
B348 | 0.25$\pm$ 0.04 | 1 |  $-1.38\pm$ 0.07 | 4
B350 | 0.10$\pm$ 0.02 | 1 |  $-1.47\pm$ 0.17 | 2
B351 | 0.15$\pm$ 0.02 | 1 |  $-1.60\pm$ 0.05 | 4
B352 | 0.14$\pm$ 0.02 | 1 |  $-1.88\pm$ 0.83 | 3
B354 | 0.05$\pm$ 0.02 | 1 |  $-1.46\pm$ 0.38 | 2
B356 | 0.31$\pm$ 0.01 | 1 |  $-1.46\pm$ 0.28 | 1
B357 | 0.12$\pm$ 0.02 | 1 |  $-0.80\pm$ 0.42 | 3
B361 | 0.11$\pm$ 0.01 | 1 |  $-1.61\pm$ 0.02 | 4
B365 | 0.19$\pm$ 0.02 | 1 |  $-1.78\pm$ 0.19 | 1
B370 | 0.34$\pm$ 0.01 | 1 |  $-1.80\pm$ 0.02 | 1
B372 | 0.20$\pm$ 0.02 | 1 |  $-1.42\pm$ 0.17 | 1
B373 | 0.10$\pm$ 0.01 | 1 |  $-0.50\pm$ 0.22 | 3
B375 | 0.29$\pm$ 0.03 | 1 |  $-1.23\pm$ 0.22 | 3
B377 | 0.16$\pm$ 0.02 | 1 |  $-2.19\pm$ 0.65 | 3
B378 | 0.14$\pm$ 0.02 | 1 |  $-1.64\pm$ 0.26 | 1
B382 | 0.10$\pm$ 0.02 | 1 |  $-1.52\pm$ 0.27 | 1
B383 | 0.00$\pm$ 0.02 | 2 |  $-0.48\pm$ 0.20 | 2
B384 | 0.04$\pm$ 0.02 | 1 |  $-0.66\pm$ 0.22 | 3
B386 | 0.21$\pm$ 0.01 | 1 |  $-1.62\pm$ 0.14 | 1
B387 | 0.12$\pm$ 0.02 | 1 |  $-1.96\pm$ 0.29 | 3
B393 | 0.14$\pm$ 0.02 | 1 |  $-1.41\pm$ 0.05 | 4
B399 | 0.03$\pm$ 0.02 | 1 |  $-1.69\pm$ 0.09 | 4
B401 | 0.06$\pm$ 0.06 | 2 |  $-1.75\pm$ 0.29 | 2
B403 | 0.07$\pm$ 0.02 | 1 |  $-0.45\pm$ 0.78 | 3
B405 | 0.14$\pm$ 0.02 | 1 |  $-1.80\pm$ 0.31 | 3
B420 | 0.30$\pm$ 0.03 | 1 |  $-0.63\pm$ 0.07 | 4
B448 | 0.05$\pm$ 0.01 | 1 |  $-2.16\pm$ 0.19 | 1
B457 | 0.14$\pm$ 0.02 | 1 |  $-1.60\pm$ 0.21 | 4
B461 | 0.58$\pm$ 0.07 | 1 |  $-2.56\pm$ 0.07 | 4
B462 | 0.39$\pm$ 0.04 | 1 |  $-2.28\pm$ 0.34 | 4
B467 | 0.27$\pm$ 0.02 | 1 |  $-2.49\pm$ 0.47 | 1
B472 | 0.13$\pm$ 0.00 | 1 |  $-1.45\pm$ 0.02 | 1
B475 | 0.16$\pm$ 0.03 | 1 |  $-2.00\pm$ 0.14 | 1
B476 | 0.08$\pm$ 0.05 | 1 |  $-0.03\pm$ 0.13 | 4
B483 | 0.08$\pm$ 0.06 | 1 |  $-2.96\pm$ 0.35 | 1
B486 | 0.17$\pm$ 0.02 | 1 |  $-2.28\pm$ 0.98 | 3
B489 | 0.17$\pm$ 0.04 | 1 |  $-0.04\pm$ 0.10 | 4
B495 | 0.34$\pm$ 0.08 | 1 |  $-0.35\pm$ 0.05 | 4
G260 | 0.30$\pm$ 0.05 | 1 |  $-2.45\pm$ 0.06 | 4

aafootnotetext: The reddening values are taken from Fan et al. (2008) (ref=1)
and Barmby et al. (2000) (ref=2).

bbfootnotetext: The metallicities are taken from Perrett et al. (2002)
(ref=1), Barmby et al. (2000) (ref=2), Huchra et al. (1991) (ref=3), and Fan
et al. (2008) (ref=4).

Table 5Ages estimates for 104 GCs and GC candidates in M31. Object | Age | $\chi_{\rm min}^{2}$ | Object | Age | $\chi_{\rm min}^{2}$
---|---|---|---|---|---
| (Gyr) | (per degree of freedom) |  | (Gyr) | (per degree of freedom)
B001 | $10.51\pm 0.80$ | 2.79 | B313 | $7.28\pm 0.70$ | 5.48
B003 | $2.01\pm 0.20$ | 2.10 | B315 | $0.50\pm 0.10$ | 7.88
B005 | $1.60\pm 0.10$ | 18.92 | B316 | $1.06\pm 0.10$ | 7.81
B018 | $1.79\pm 0.20$ | 2.74 | B317 | $2.06\pm 0.15$ | 2.59
B020D | $8.41\pm 1.70$ | 1.29 | B325 | $0.40\pm 0.10$ | 5.28
B024 | $15.25\pm 0.75$ | 2.96 | B332D | $11.30\pm 0.85$ | 4.33
B046 | $1.30\pm 0.10$ | 5.71 | B335 | $1.17\pm 0.15$ | 3.55
B058 | $2.02\pm 0.10$ | 2.41 | B337 | $2.03\pm 0.10$ | 5.66
B083 | $2.89\pm 0.20$ | 10.25 | B338 | $1.70\pm 0.10$ | 2.43
B085 | $2.18\pm 0.20$ | 2.39 | B340D | $13.57\pm 1.45$ | 9.68
B138D | $2.95\pm 0.35$ | 8.09 | B343 | $1.82\pm 0.10$ | 2.82
B140D | $0.39\pm 0.10$ | 12.18 | B344 | $12.68\pm 2.35$ | 2.60
B141D | $4.76\pm 1.00$ | 3.78 | B347 | $2.53\pm 0.15$ | 3.23
B142D | $0.03\pm 0.01$ | 18.34 | B348 | $6.58\pm 0.70$ | 3.28
B144D | $14.36\pm 0.95$ | 3.36 | B350 | $1.99\pm 0.10$ | 2.25
B156D | $0.10\pm 0.01$ | 22.86 | B351 | $3.20\pm 0.40$ | 2.26
B157D | $8.00\pm 1.05$ | 3.81 | B352 | $1.51\pm 0.10$ | 1.16
B165D | $0.50\pm 0.10$ | 20.62 | B354 | $5.24\pm 0.65$ | 3.85
B166D | $3.73\pm 0.90$ | 3.26 | B356 | $1.21\pm 0.10$ | 3.16
B167D | $0.90\pm 0.10$ | 3.22 | B357 | $4.98\pm 0.60$ | 2.94
B172D | $1.00\pm 0.10$ | 10.73 | B361 | $1.57\pm 0.10$ | 1.40
B177D | $1.70\pm 0.30$ | 3.32 | B365 | $1.73\pm 0.10$ | 1.89
B181D | $0.63\pm 0.15$ | 7.72 | B370 | $1.10\pm 0.10$ | 3.17
B196 | $1.62\pm 0.10$ | 2.39 | B372 | $2.34\pm 0.35$ | 1.54
B223D | $4.03\pm 0.35$ | 6.13 | B373 | $7.79\pm 0.40$ | 1.02
B240 | $1.79\pm 0.10$ | 1.05 | B375 | $2.19\pm 0.30$ | 7.62
B244 | $0.90\pm 0.10$ | 6.33 | B377 | $1.09\pm 0.10$ | 1.81
B245D | $0.10\pm 0.01$ | 7.58 | B378 | $2.12\pm 0.30$ | 3.70
B257 | $0.10\pm 0.01$ | 6.16 | B382 | $1.83\pm 0.15$ | 3.33
B260 | $14.30\pm 0.50$ | 1.26 | B383 | $13.99\pm 1.05$ | 4.73
B261D | $0.57\pm 0.10$ | 6.91 | B384 | $10.27\pm 0.95$ | 4.29
B266 | $0.03\pm 0.01$ | 10.36 | B386 | $2.54\pm 0.15$ | 1.93
B270D | $1.00\pm 0.10$ | 4.01 | B387 | $1.62\pm 0.10$ | 2.66
B272 | $3.73\pm 0.90$ | 5.10 | B393 | $6.76\pm 1.10$ | 1.17
B281 | $5.97\pm 1.30$ | 1.97 | B399 | $5.59\pm 0.50$ | 2.03
B283D | $1.09\pm 0.10$ | 3.84 | B401 | $3.49\pm 0.40$ | 2.55
B283 | $2.83\pm 0.35$ | 4.99 | B403 | $6.39\pm 0.40$ | 2.56
B289D | $0.81\pm 0.25$ | 2.20 | B405 | $1.30\pm 0.10$ | 2.97
B292D | $1.15\pm 0.15$ | 4.49 | B420 | $10.90\pm 0.40$ | 4.86
B292 | $1.00\pm 0.10$ | 2.53 | B448 | $1.70\pm 0.10$ | 6.19
B293D | $0.50\pm 0.10$ | 3.90 | B457 | $3.16\pm 0.35$ | 12.00
B297D | $15.18\pm 0.85$ | 3.37 | B461 | $0.56\pm 0.10$ | 9.51
B301 | $2.20\pm 0.30$ | 4.06 | B462 | $0.50\pm 0.10$ | 4.38
B303 | $0.50\pm 0.10$ | 17.86 | B467 | $1.00\pm 0.10$ | 5.95
B304 | $2.20\pm 0.10$ | 1.36 | B472 | $1.30\pm 0.10$ | 5.15
B305 | $0.40\pm 0.10$ | 9.52 | B475 | $0.97\pm 0.10$ | 6.69
B306 | $3.39\pm 0.50$ | 4.61 | B476 | $3.14\pm 0.35$ | 7.65
B307 | $1.61\pm 0.10$ | 7.46 | B483 | $1.00\pm 0.10$ | 6.49
B309 | $4.66\pm 0.55$ | 10.39 | B486 | $1.61\pm 0.10$ | 3.31
B310 | $2.07\pm 0.15$ | 1.35 | B489 | $9.07\pm 1.30$ | 3.56
B311 | $1.62\pm 0.10$ | 4.21 | B495 | $14.54\pm 0.55$ | 2.81
B312 | $2.56\pm 0.25$ | 7.27 | G260 | $1.00\pm 0.10$ | 5.84
Table 6Age comparison Object | Age (Gyr) | Age (Gyr)
---|---|---
| (Caldwell et al., 2009) | (this paper)
B018 | 1.00 | $1.79\pm 0.20$
B303 | 0.40 | $0.50\pm 0.10$
B307 | 1.00 | $1.61\pm 0.10$
B315 | 0.16 | $0.50\pm 0.10$
B316 | 1.00 | $1.06\pm 0.10$
B325 | 0.63 | $0.40\pm 0.10$
B448 | 0.25 | $1.70\pm 0.10$
B475 | 0.32 | $0.97\pm 0.10$
B483 | 0.50 | $1.00\pm 0.10$