| Home |
|
| Where to Start |
|
| About DR6 |
|
| News and Updates |
|
| Tutorials |
|
| Data Products |
|
| Data Access |
|
| Sky Coverage |
|
| Instruments |
|
| Data Flow |
|
| Algorithms |
|
| Glossary |
|
| Known Problems |
|
| Help and Feedback |
|
| Search |
 |
 |
The SEGUE Stellar Parameter Pipeline 'sppLines' TableUp to SpectraSpectra for over 250,000 Galactic stars of all common spectral types are available with DR6. These Spectra were processed with a pipeline called the 'SEGUE Stellar Parameter Pipeline' (sspp) which computes line indices for a wide range of common features at the radial velocity of the star in question. These outputs are stored in the CAS in a table called 'sppLines', indexed on the 'specObjID' key index parameter for queries joining to other tables such as specobjall and photoobjall. The fields available in the sppLines table in the CAS (also see sppLines description in CAS schema browser) are:
The star is identified with these numbers:
specobjid int64 Unique spectrum id f(plate,mjd,fiberid) bigint(8 bytes)
plate int
mjd int
fiberid int
Then for each star, for each index below,
the 'side band' EqW (A) and the 'continuum' EqW (A) along with an
Error (A) and a mask (0=bad, 1=ok) value are tablulated:
The name of the index, the central wavelength and width of the
on and off bands are recorded here (in Angstroms).
Index_name Lambda0 Width Upper_refband width Lower_ref width
----------------------------------------------------------------
H8w3 3889.0 3.0 3912.0 8.0 3866.0 8.0
H8w12 3889.1 12.0 4010.0 20.0 3862.0 20.0
H8w24 3889.1 24.0 4010.0 20.0 3862.0 20.0
H8w48 3889.1 48.0 4010.0 20.0 3862.0 20.0
KPw12 3933.7 12.0 4010.0 20.0 3913.0 20.0
KPw18 3933.7 18.0 4010.0 20.0 3913.0 20.0
KPw6 3933.7 6.0 4010.0 20.0 3913.0 20.0
CaIIK 3933.6 30.0 4010.0 5.0 3910.0 5.0
CaIIHKp 3962.0 75.0 4010.0 5.0 3910.0 5.0
Heps 3970.0 50.0 4010.0 5.0 3910.0 5.0
KPw16 3933.7 16.0 4018.0 20.0 3913.0 10.0
Sr 4077.0 8.0 4090.0 6.0 4070.0 4.0
HeI 4026.2 12.0 4154.0 20.0 4010.0 20.0
Hdeltaw12 4101.8 12.0 4154.0 20.0 4010.0 20.0
Hdeltaw24 4101.8 24.0 4154.0 20.0 4010.0 20.0
Hdeltaw48 4101.8 48.0 4154.0 20.0 4010.0 20.0
Hdelta 4102.0 64.0 4154.0 20.0 4010.0 20.0
CaI 4226.0 4.0 4232.0 4.0 4211.0 6.0
CaIw12 4226.7 12.0 4257.0 20.0 4154.0 20.0
CaIw24 4226.7 24.0 4257.0 20.0 4154.0 20.0
CaIw6 4226.7 6.0 4257.0 20.0 4154.0 20.0
G 4305.0 15.0 4367.0 10.0 4257.0 20.0
Hgammaw12 4340.5 12.0 4425.0 20.0 4257.0 20.0
Hgammaw24 4340.5 24.0 4425.0 20.0 4257.0 20.0
Hgammaw48 4340.5 48.0 4425.0 20.0 4257.0 20.0
Hgamma 4340.5 54.0 4425.0 20.0 4257.0 20.0
HeIa 4471.7 12.0 4500.0 20.0 4425.0 20.0
G_blue 4305.0 26.0 4507.0 14.0 4090.0 12.0
G_whole 4321.0 28.0 4507.0 14.0 4096.0 12.0
Ba 4554.0 6.0 4560.0 4.0 4538.0 4.0
12C13C 4737.0 36.0 4770.0 20.0 4423.0 10.0
CC12 4618.0 256.0 4780.0 5.0 4460.0 10.0
metal1 4584.0 442.0 4805.8 5.0 4363.0 5.0
Hbetaw12 4862.3 12.0 4905.0 20.0 4790.0 20.0
Hbetaw24 4862.3 24.0 4905.0 20.0 4790.0 20.0
Hbetaw48 4862.3 48.0 4905.0 20.0 4790.0 20.0
Hbeta 4862.3 60.0 4905.0 20.0 4790.0 20.0
C2 5052.0 204.0 5230.0 20.0 4935.0 10.0
C2+MgI 5069.0 238.0 5230.0 20.0 4935.0 10.0
MgH+MgI+C2 5085.0 270.0 5230.0 20.0 4935.0 10.0
MgH+MgI 5198.0 44.0 5230.0 20.0 4935.0 10.0
MgH 5210.0 20.0 5230.0 20.0 4935.0 10.0
CrI 5206.0 12.0 5239.0 8.0 5197.5 5.0
MgI+FeII 5175.0 20.0 5240.0 10.0 4915.0 10.0
MgI 5183.0 2.0 5240.0 10.0 4915.0 10.0
MgIa 5170.5 12.0 5285.0 20.0 5110.0 20.0
MgIb 5176.5 24.0 5285.0 20.0 5110.0 20.0
MgIc 5183.5 12.0 5285.0 20.0 5110.0 20.0
NaI 5890.0 20.0 5918.0 6.0 5865.0 10.0
Naw12 5892.9 12.0 5970.0 20.0 5852.0 20.0
Naw24 5892.9 24.0 5970.0 20.0 5852.0 20.0
Halphaw12 6562.8 12.0 6725.0 50.0 6425.0 50.0
Halphaw24 6562.8 24.0 6725.0 50.0 6425.0 50.0
Halphaw48 6562.8 48.0 6725.0 50.0 6425.0 50.0
Halphaw70 6562.8 70.0 6725.0 50.0 6425.0 50.0
CaH 6788.0 505.0 7434.0 10.0 6532.0 5.0
TiO 7209.0 333.3 7434.0 10.0 6532.0 5.0
CN 6890.0 26.0 7795.0 10.0 6870.0 10.0
OItrip 7775.0 30.0 7805.0 10.0 7728.0 10.0
KI 7687.0 34.0 8080.0 10.0 7510.0 10.0
KIa 7688.0 95.0 8132.0 5.0 7492.0 5.0
NaIa 8187.5 15.0 8190.0 55.0 8150.0 10.0
NaIred 8190.2 33.0 8248.6 5.0 8140.0 5.0
CaIIw26 8498.0 26.0 8520.0 10.0 8467.5 25.0
Paschenw13 8467.5 13.0 8570.0 14.0 8457.0 10.0
CaII 8498.5 29.0 8570.0 14.0 8479.0 10.0
CaIIw40 8542.0 40.0 8570.0 14.0 8479.0 10.0
CaIIa 8542.0 16.0 8600.0 60.0 8520.0 20.0
Paschenw42 8598.0 42.0 8630.5 23.0 8570.0 14.0
CaIIb 8662.1 16.0 8694.0 12.0 8600.0 60.0
CaIIaw40 8662.0 40.0 8712.5 25.0 8630.5 23.0
Paschenaw42 8751.0 42.0 8784.0 16.0 8712.5 25.0
TiO5 7134.4 5.0 7134.4 5.0 7045.9 4.0
TiO8 8457.3 30.0 8457.3 30.0 8412.3 20.0
CaH1 6386.7 10.0 6415.0 10.0 6351.7 10.0
CaH2 6831.9 32.0 7045.9 4.0 7045.9 4.0
CaH3 6976.9 30.0 7045.9 4.0 7045.9 4.0
------------------------------------------------------------------
Try sending this query:
select top 10 * from sppLines
to get a feel for the columns.
Here's a sample query which selects red stars (spectral type K)
that are bright (g0 < 17), with large CaII triplet eq widths, with low errors
on the CaII triplet eq widths:
select sp.plate,sp.mjd,sp.fiberid,sp.g0,sp.gmr0,
sl.caII,sl.caIIerr,sl.caIIa,sl.caIIaerr,
sl.caIIb,sl.caIIberr,sl.caII+sl.caIIa+sl.caIIb as caIItripsum,
sp.feha,sp.fehaerr,sp.fehan,sp.logga,sp.loggaerr,sp.loggan
from sppLines as sl, sppParams as sp where
sl.CaII + sl.CaIIa + sl.CaIIb > 12 and
sl.CaIImask = 1 and sl.CaIIamask =1 and
sl.CaIIbmask = 1 and sl.caIIerr < 2 and
sl.caIIaerr < 2 and sl.caIIberr < 2 and
sl.caII > 0 and sl.caIIa > 0 and sl.caIIb > 0 and
gmr0 between 0.8 and 1.1
and g0 < 17
and sl.specobjid = sp.specobjid
(returns 5 stars).
Last modified: Tue Jun 26 14:52:41 CEST 2007 |