98 research outputs found
The Correlations between the Intrinsic Colors and Spectroscopic Metallicities of M31 Globular Clusters
We present the correlations between the spectroscopic metallicities and
ninety-three different intrinsic colors of M31 globular clusters, including
seventy-eight BATC colors and fifteen SDSS and near infrared ugrizK colors. The
BATC colors were derived from the archival images of thirteen filters (from c
to p), which were taken by Beijing-Arizona-Taiwan-Connecticut (BATC) Multicolor
Sky Survey with a 60/90 cm f/3 Schmidt telescope. The spectroscopic
metallicities adopted in our work were from literature. We fitted the
correlations of seventy-eight different BATC colors and the metallicities for
123 old confirmed globular clusters, and the result implies that correlation
coefficients of twenty-three colors r>0.7. Especially, for the colors
, , and , the correlation coefficients are r>0.8.
Meanwhile, we also note that the correlation coefficients (r) approach zero for
, , , and , which are likely to be
independent of metallicity. Similarity, we fitted the correlations of
metallicity and ugrizK colors for 127 old confirmed GCs. The result indicates
that all these colors are metal-sensitive (r>0.7), of which is the
most metal-sensitive color. Our work provides an easy way to simply estimate
the metallicity from colors.Comment: 25 pages, 11 figures, 2 tables, accepted for publication in PASP
Determination of fundamental properties of an M31 globular cluster from main-sequence photometry
M31 globular cluster B379 is the first extragalactic cluster, the age of
which was determined by main-sequence photometry. In this method, the age of a
cluster is obtained by fitting its CMD with stellar evolutionary models.
However, different stellar evolutionary models use different parameters of
stellar evolution, such as range of stellar masses, different opacities and
equations of state, and different recipes, and so on. So, it is interesting to
check whether different stellar evolutionary models can give consistent results
for the same cluster. Brown et al. (2004a) constrained the age of B379 by
comparing its CMD with isochrones of the 2006 VandenBerg models. Using SSP
models of BC03 and its multi-photometry, Ma et al. (2007) independently
determined the age of B379, which is in good agreement with the determination
of Brown et al. (2004a). The BC03 models are calculated based on the Padova
evolutionary tracks. It is necessary to check whether the age of B379 which,
being determined based on the Padova evolutionary tracks, is in agreement with
the determination of Brown et al. (2004a). So, in this paper, we re-determine
its age using isochrones of the Padova stellar evolutionary models. In
addition, the metal abundance, the distance modulus, and the reddening value
for B379 are also determined in this paper. The results obtained in this paper
are consistent with the previous determinations, which including the age
obtained by Brown et al. (2004a). So, this paper confirms the consistence of
the age scale of B379 between the Padova isochrones and the 2006 VandenBerg
isochrones, i.e. the results' comparison between Brown et al. (2004a) and Ma et
al. (2007) is meaningful. The results obtained in this paper are: the
metallicity [M/H]=-0.325, the age Gyr, the reddening value
E(B-V)=0.08, and the distance modulus .Comment: Accepted for Publication in PASP, 7 pages, 1 figure and 1 tabl
Spectral Energy Distributions of M81 Globular Clusters in BATC Multicolor Survey
In this paper, we give the spectral energy distributions of 42 M81 globular
clusters in 13 intermediate-band filters from 4000 to 10000 A, using the CCD
images of M81 observed as part of the BATC multicolor survey of the Sky. The
BATC multicolor filter system is specifically designed to exclude most of the
bright and variable night-sky emission lines including the OH forest. Hence, it
can present accurate SEDs of the observed objects. These spectral energy
distributions are low-resolution spectra, and can reflect the stellar
populations of the globular clusters. This paper confirms the conclusions of
Schroder et al. that, M81 contains clusters as young as a few Gyrs, which also
were observed in both M31 and M33Comment: Accepted for Publication in PASP, 10 pages, 3 figure
Evolution of Galaxy Luminosity Function and Luminosity Function by Density Environment at 0.03<z<0.5
Using galaxy sample observed by the BATC large-field multi-color sky survey
and galaxy data of SDSS in the overlapped fields, we study the dependence of
the restframe -band galaxy luminosity function on redshift and on
large-scale environment. The large-scale environment is defined by isodensity
contour with density contrast \delta\rho/\rho. The data set is a composite
sample of 69,671 galaxies with redshifts 0.03 < z < 0.5 and r < 21.5 mag. The
redshifts are composed by three parts: 1) spectroscopic redshifts in SDSS for
local and most luminous galaxies; 2) 20-color photometric redshifts derived
from BATC and SDSS; 3) 5-color photometric redshifts in SDSS. We find that the
faint-end slope \alpha steepens slightly from -1.21 at z ~ 0.06 to -1.35 at z ~
0.4, which is the natural consequence of the hierarchical formation of
galaxies. The luminosity function also differs with different environments. The
value of \alpha changes from -1.21 at underdense regions to -1.37 at overdense
regions and the corresponding M* brightens from -22.26 to -22.64. This suggests
that the fraction of faint galaxies is larger in high density regions than in
low density regions.Comment: 7 pages, 9 figures, accepted by Ap
Optical Photometry of Type II-P Supernova 2004dj in NGC 2403
We present photometric data of the type II-P supernova (SN) 2004dj in NGC
2403. The multicolor light curves cover the SN from 60 to 200 days after
explosion, and are measured with a set of intermediate-band filters that have
the advantage of tracing the strength variations of some spectral features. The
light curves show a flat evolution in the middle of the plateau phase, then
decline exponentially at the late times, with a rate of 0.100.03 mag (10
days) in most of the filters. In the nebular phase, the spectral energy
distribution (SED) of SN 2004dj shows a steady increase in the flux near 6600
\AA and 8500 \AA, which may correspond to the emission lines of H and
Ca II near-IR triplet, respectively. The photometric behavior suggests that SN
2004dj is a normal SN II-P. Compared with the light curves of another typical
SN II-P 1999em, we estimate the explosion date to be June 1021 UT, 2004
(JD 245316721) for SN 2004dj. We also estimate the ejected nickel mass
during the explosion to be = 0.023 0.005
from two different methods, which is typical for a SN II-P. We derive the
explosion energy erg, the ejecta
mass , and the initial radius for the presupernova star of SN 2004dj,
which are consistent with other typical SNe II-P.Comment: 15 pages, 9 figures, accepted for publication in A
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