star counts and the galactic structure xu yan supervisor: deng li cai
TRANSCRIPT
Star Counts and The Galactic Structure
Xu Yan
Supervisor: Deng Li Cai
Introduction
Sloan digital sky survey Synthetic star counts model Future plan
Sloan Digital Sky Survey
Five broad band filters,u’,g’,r’,i’,z’
effective wavelengths, 3450Å, 4760Å, 6280Å, 7690Å,9250Å
point-source magnitude limit, 22.3, 23.3, 23.1, 22.3, 20.8 (s/n=5)
Pixels subtend 0”.4, PSF width1.4" median in r Exposure time in each band is 54.1s ‘run’, six 13’.5 wide strips, ‘rerun’, 12’.5
2o.5 wide stripe (Chen et. al. 2001)
45 survey stripes
DR2 Sky Coverage 3324 sq deg Equatorial
http://www.sdss.org/dr2/coverage/index.html
DR2 Sky Coverage Galactic
http://www.sdss.org/dr2/coverage/index.html
Synthetic model
ρ(R,Z), Φ(Mass) → surface number density of some direction of some population
each population → [Fe/H], Mass, Age From Isochrone → [Fe/H], Teff, g Color of each star
Robin(2003)group
Age(Gyr) [Fe/H](dex) IMF ρ0(MΘPC-3)
1 0 – 0.15 0.010.12 dn/dm=m-1.6
(M<1MΘ)
dn/dm=m-3
(M≥1MΘ)
4*10-3
2 0.15 - 1 0.030.12 7.9*10-3
3 1 - 2 0.030.1 6.2*10-3
4 2 - 3 0.010.11 4*10-3
5 3 - 5 -0.070.18 5.8*10-3
6 5 - 7 -0.140.17 4.9*10-3
7 7 - 10 -0.370.2 6.6*10-3
8 11 -0.780.3 dn/dm=m-0.5 1.34*10-3
9 14 -1.780.5 9.32*10-3
91
22
1
)()(
)(,
AAA
dRRdMassRdMassA
MassPMFZRdAMass
Mass R
i
i
]/||exp[]/)(exp[),( 2100 hzhrxMrd
87
4/1
0
])/(exp[
e
es
rr
rrbCsr
)()( massIMFmass
Chen (2001)
Bahcall(1980)
5.02
36.11
)(
)()(
mcM
mmcMRobin(2003)
PMF ~ IMF Mass density convert to number density
is normalized IMF
Logz=1.03[Fe/H]-1.689 (Carraro et. al. 1994) z, Age, Mass
dm
dn
dmdm
dnmcymassdenist dm
dm
dncnumdensity
Pseudo-random in age and metalicity
Group1,Mass: 0.1505000D+00 0.1515000D+00 (M☉)
The tables of bolometric corrections have been applied to Padova database of stellar evolutionary tracks and isochrones. http://pleiadi.pd.astro.it.
Interpolate in SDSS Isochrone of Giradi(2004) and Ma(2001)
0
02
1
2
1log5.2
Ss m
dSf
dSf
m
SbolS MMBC
0
0
4.0
2,
2
1
2
1
10
log5.2
]/)10(4log[5.2
S
A
bolbolS
m
dSf
dSF
LFpcMBC
Stellar spectra Fλ , spectral library
'1'0 2/sinhlog5.2 bfabmf
ea log5.2
'0 log5.20 bm
Lupton et al (1999)
fmfm log5.2)( 0
AB magnitude scale
00, ABm
121200, 10631.3 Hzcmsergf AB
u-g g-r r-I i-z
107 , 10 8,109,1010 yr (Giradi 2004)
12Gyr, z=0.0001,0.0004,0.001,0.004,0.008,0.019,0.03 (Giradi2004)
isoc_sloan/isoc_z0.dat.gz Metal-free models from Ma01.
isoc_sloan/isoc_z0001.dat.gz isoc_sloan/isoc_z0004.dat.gz isoc_sloan/isoc_z001.dat.gz isoc_sloan/isoc_z004.dat.gz isoc_sloan/isoc_z008.dat.gz isoc_sloan/isoc_z019.dat.gz
isoc_sloan/isoc_z030.dat.gz
Basic set obtained by combining Gi00+Gi01 (low- and intermediate-mass stars) with Be94+Gi96 (high masses) isochrones. With overshooting
R=50PC z=41.44PC
Ra=180 dec=60 skycoverage=1srL=134.4 b=55.97
R=150PC z=124.31PC
R=250PC z=207.186PC
R=350PC z=290.06PC
Mass(M ) Log(age) group z logT logg☉ u g r u-g g-r 0.200000 9.76540 61 0.0233971 3.62080 2.98324 6.95622 4.73258 3.71290 2.22364 1.01968. 0.200000 9.83367 61 0.0131369 3.61070 3.21589 7.97221 5.66942 4.60236 2.30279 1.06706.
R=450PC z=372.94PC
Mass(M☉) Log(age) group z logT logg u g r u-g g-r0.200000 9.19340 31 0.0124033 3.63555 3.41523 7.13436 4.98482 4.02208 2.14954 0.962740 0.200000 9.75101 61 0.0118220 3.63816 3.01763 6.46198 4.38647 3.44567 2.07551 0.940800 0.200000 9.71720 61 0.0124870 3.62821 3.20643 7.34673 5.19215 4.20510 2.15458 0.987050
R=550PC z=455.81PC
R=650PC z=538.68
R=750PC z=621.56PC
R=850PC z=704.43PC
R=950PC z=787.37PC
Classify metallicity z>0.019 0.019>z>0.004 z<0.004
Classify age
Age<12Gyr 5Gyr<Age<12Gyr Age<5Gyr
RA=180 DEC=60 33289
Compare result of model with observation
4422
Future plan
Constrain model with observation Do further deducing for physical parameter
of observational data to obtain distance Pick up stars that have special meaning to
the structure of the Galaxy
Thank you!