India Processing Tomato Segment: Current Status, Trends and ...
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Processing Status
June 2009
Mar
y W
illi
ams
Pad
ova
Mee
ting
, 11/
06/0
9
Talk OutlineM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
•Archive status
•Data flow
•New Status Reports
•Zero-points
•FP3
•Stellar parameters: temperatures
Archive statusM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
As of 9th June 2009
•285,503 spectra
•Last date in internal and reduced archives: 20090328
•Last date in raw archive: 20090328
Sky Coverage M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
First year data
25,689 RVs, ~4,500 deg2
Sky Coverage M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Second year data
26,906 RVs, ~5,000 deg2
Sky Coverage M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Third year data
37,292 RVs, ~8,800 deg2
Sky Coverage M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Fourth year data
87,261 RVs, ~17,200 deg2
Sky Coverage M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Fifth year data
41,002 RVs, ~11,000 deg2
Sky Coverage M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Sixth year data
59,945 RVs, ~11,000 deg2
Sky Coverage M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Full database
218,100 RVs, ~32,000 deg2
Current data flow M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
SSO AAO
(Warren)
PadovaReduction
(Alessandro)
AIP Archive
AIP Pipeline(Mary)
AIPProcessed
Data Archive
Problem fields
Fortnightly 3-4 days
Internal release(at AIP)
Reduction problem fields
Fortnightly
Weekly
Eyeballing of spectra(Rachel, Tomaz, Gal, Paola)
Complete to Dec 2007
1/2 weekIrregular
AIP archive
Last release complete to March 2009
New status reportsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
New status reportsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
New status reportsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
New status reportsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
New status reportsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
What are they?•Temperature fluctuations cause shift in wavelength between science frames and arc frames•Mostly of the order of a 1-5 km/s•We correct with zero-point RVcorrection•ZeroPointQualityFLAG denotes quality of zero-point correction - mostly!!
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
How do we calculate the correction?
Un-sky subtracted spectra
from single fibreSky template
SkyRV, eSkyRV, R for single fibre
THEN….
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
THEN we do a polynomial fit across the field
SkyRV and eSkyRVExclusive
sky fibre
(weight=5xR)
Weight by R value
Threshold of R=5 The fit gives RVcorrection
ZeroPointQualityFLAG gives the quality of the fit•1st character: FIELD fit quality
Dispersion between SkyRV - RVcorrection
•2nd character: Sub-group fit quality
Dispersion between SkyRV - Rvcorrection for
regions 1-50, 51-100, 101-150•*: If interval between usable sky velocities > 15
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
The fit can sometimes be very bad…
Fiorangela La Forgia
It can become unbound if there are insufficient fibres with R>5
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Sometimes bad zero-points are hard to spot
•X-correlation with sky has |50| km/s limit•If outside those bounds
SkyRV=0, eSkyRV=0 or large, R<0.1•The RVs for such spectra can be wrong by as much as 100 km/s! •Affects small number of fields•These data are removed from the database
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
The other bad fits are hand corrected•All zero-points fits are eyeballed•Those with unbound fits are manually corrected•New flagging of affected spectra:
ZeroPointQualityFLAG=‘M’ •However, there has been an increase in problem fields…
Fiorangela La Forgia
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
There were a number of causes of this increase•Shift to brighter stars, lower exposure time
Exposure times increased back again•Poor placement of sky fibres
More care taken•Deterioration of fibres meaning lower S/N
FP3
There is a backlog of correcting these fits
manually•Be wary if |RVcorrection| > 10 km/s or *!•If find some high RV stars, check fellow fibres
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Correlation between RV and SkyRV•Caused by underlying stellar spectrum “tugging” on
sky correlation
•Not a problem for zero point calibration IF there is
no mean offset in stellar RVs for one field…BUT…
Zero-pointsM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
There might be such a issue
•Whole fields have have a non-zero mean RV •Causes shift in Rvcorrectionof the order of a coupleof kms-1
•Work in progress
Field Plate 3M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
The first 8 FP3 fields•New stiffer cabling used - potential problems!•Check stability of SkyRV
Grey : R < 5Black: R > 5
Field Plate 3M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Stability of SkyRV for R > 5•FP3: (SkyRV)=-0.5 kms-1, (SkyRV)=1.9 kms-1
•FP1: (SkyRV)=-0.4 kms-1, (SkyRV)=2.9 kms-1
•FP2: (SkyRV)=-0.4 kms-1, (SkyRV)=2.2 kms-1
Field Plate 3M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Some of the fields include repeat observations
All but one field look good
Field Plate 3M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
The problem field was one of the earlier ones
So ignoring this field and |RV(FP3) - RV(previous)| < 20 kms-1
Field Plate 3M
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Stability of SkyRV for R > 5•FP3: (RP3 RV-previous RV)=-0.5 kms-1
68.2%: =1.1 kms-1 95%: =2.3 kms-1
•ALL: (RP3 RV-previous RV)=+0.2 kms-1
68.2%: =1.4 kms-1 95%: =3.8 kms-1
Stellar ParametersM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
Comparing RAVE temperatures to others
•To spot any possible systematic in RAVE temperatures•Use a variety of reference temperatures:
Photometric: V-K using Ramirez calibrations with reddening corrections and constraintsJon’s spectroscopic temperatures: excitation balanceSoubiran and Girard temperatures: photometric, excitation balance, H
Cayrel compilation temperatures: photometric, H
•Thus we have a broad range of methods to compare our temperature calculations to
Stellar ParametersM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
There is a significant systematic for the dwarfs
GREEN - V-K photometricBLACK - Jon’s calculationCYAN - Soubiran and GirardPURPLE - Cayrel
Stellar ParametersM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
It remains at higher S/N values
GREEN - V-K photometricBLACK - Jon’s calculationCYAN - Soubiran and GirardPURPLE - Cayrel
SummaryM
ary
Wil
liam
s P
adov
a M
eeti
ng, 1
1/06
/09
•Processing continuing as normal
•New status reports to aid dissemination of data and
identification of problems
•Zero-pointsRemoval of bad fields
Manual refitting backlog: watch out!
Possible problem with star RV correlation - investigating
•FP3Sky RVs good
Repeats good, apart from mean offset - investigating
New report out soon
•Possible temperature systematic