Progress report on analysis and calibration of RAVE data and preparation for DR3 · 2009. 6....

Tomaž Zwitter: RAVE, Padova workshop, 11/6/2009 Tomaž Zwitter: RAVE, Padova workshop, 11/6/2009 11

Tomaž ZwitterTomaž Zwitter

University of LjubljanaUniversity of LjubljanaFaculty of Mathematics and PhysicsFaculty of Mathematics and Physics

Progress report on analysis and calibration Progress report on analysis and calibration of RAVE data and preparation for DR3of RAVE data and preparation for DR3

3rd field plate


Plan:Plan:

FP3FP3 RVsRVs Stellar parametersStellar parameters DistancesDistances DR3 preparationDR3 preparation DR4+DR4+

Progress report on analysis and calibration Progress report on analysis and calibration of RAVE data and preparation for DR3of RAVE data and preparation for DR3

3rd field plate


FP3 performanceFP3 performance3rd field plate

FP3 resultsFP3 results (Mary): (Mary):summary: very goodsummary: very good

FP3 performanceFP3 performance (Fred): (Fred): Fiber lifetime: very goodFiber lifetime: very goodMechanics: ok, caution on cable & slitMechanics: ok, caution on cable & slit


Reduction pipelineReduction pipeline

Fred & observers

Paul

Warren

Alessandro Mary

InputCatalogGroup

DataManagement

Group

checking...

Actually everybody Actually everybody connected toconnected toeverybody else. everybody else.


Number of pointingsNumber of pointings

~350.000 spectra covering ~17.000 square degrees ~350.000 spectra covering ~17.000 square degrees ~20 objects/degree~20 objects/degree22 on average, maximum is 107 spectra/degree on average, maximum is 107 spectra/degree22..


Measured radial velocitiesMeasured radial velocities


Radial Radial velocityvelocityerrorserrors


Radial velocity shiftsRadial velocity shiftsUncontrolled shifts in wavelength calibration.Uncontrolled shifts in wavelength calibration. Affects 5 whole fields and in addition the fibers 3-9 in 66 fieldsAffects 5 whole fields and in addition the fibers 3-9 in 66 fieldsin DR3.in DR3.Solution: Solution: - few fields & few fiber 3-9 ranges with really bad RVs are removed,- few fields & few fiber 3-9 ranges with really bad RVs are removed,- the user needs to be suspicious of and RV corrections >10 km/s.- the user needs to be suspicious of and RV corrections >10 km/s.


Radial velocity definition: Radial velocity definition: gravitational redshift not includedgravitational redshift not included

v = GM / Rc =v = GM / Rc = = 0.636 km/s ( M/M= 0.636 km/s ( M/Mּס ּס ) ( R/R) ( R/Rּס ּס ))

-1-1

∇∇p = - p = - ρ ρ g , g = GM / R g , g = GM / R2 2 M and R enter stellar atmosphere M and R enter stellar atmosphere calculation through:calculation through:

Gravitational redshift of light Gravitational redshift of light leaving the stellar surface:leaving the stellar surface:

> From: [email protected]> Date: June 5, 2009 12:12:30 AM GMT+02:00

> Dear Urtzi,> SYNTHE always computes in the laboratory rest frame because the line > data are in the laboratory frame... That way I can check wavelengths > against laboratory line lists without having to think about red shifts.


Radial velocity definition: Radial velocity definition: gravitational redshift not includedgravitational redshift not included

Morales-Rueda et al. 2005

Example: A white dwarf + M dwarf binary. Example: A white dwarf + M dwarf binary.


Check with repeated observationsCheck with repeated observations

19 May 2009 internal data release:19 May 2009 internal data release: ∆∆ RV = 1.8 km/sRV = 1.8 km/s276024 spectra, 276024 spectra, ∆∆ Teff = 135 K Teff = 135 K 241376 objects observed once, 241376 objects observed once, ∆∆ log g = 0.2 dex,log g = 0.2 dex,15730 more than once 15730 more than once ∆∆ [M/H] = 0.1 dex[M/H] = 0.1 dex

These errors on stellar parameters are These errors on stellar parameters are less than halfless than half of what is of what isderived from comparison with external datasets. So external datasetsderived from comparison with external datasets. So external datasetsvalues may not be error free and RAVE errors are indeed smaller.values may not be error free and RAVE errors are indeed smaller.

If If ∆∆ RV > 5 km/s this is likely due to binarity (single lined spectroscopic RV > 5 km/s this is likely due to binarity (single lined spectroscopic binary). This happens in 6% of the cases. In binary). This happens in 6% of the cases. In ~0.6~0.6% binarity in a form % binarity in a form of a double lined spectroscopic binary detected from a single spectrum. of a double lined spectroscopic binary detected from a single spectrum.


Errors for repeated observationsErrors for repeated observations


A

re parameter values reliable?

Are param

eter values reliable?L

ast r

epor

t by

Cor

rado

& M

ary

(25-

May

-200

9)


Are parameter values reliableAre parameter values reliable(within limits expected for a dataset of this kind)(within limits expected for a dataset of this kind)??

Two cases: low S/N spectra, high S/N spectra.Two cases: low S/N spectra, high S/N spectra. Low S/N: everybody agrees, will be discussed later.Low S/N: everybody agrees, will be discussed later. High S/N: no (Corrado, Mary)High S/N: no (Corrado, Mary)

yes (Ulisse, Tomaz, Jon)yes (Ulisse, Tomaz, Jon)

Arguments to be presented during this meeting:Arguments to be presented during this meeting: Comparison with synthetic spectra, with Soubiran&Girard sampleComparison with synthetic spectra, with Soubiran&Girard sample and observations of clusters using modified (how?) RAVE pipeline and observations of clusters using modified (how?) RAVE pipeline to reduce them (Mary, Corrado).to reduce them (Mary, Corrado). High-res tests (Jon), tests on repeats (Jon), High-res tests (Jon), tests on repeats (Jon), better metallicity calibration (Jon).better metallicity calibration (Jon). Tests on temperature and metallicity using reliably Tests on temperature and metallicity using reliably classified HD stars (Ulisse), customary observations (Ulisse).classified HD stars (Ulisse), customary observations (Ulisse). Comments on theoretical spectra and their culprits (Urtzi). Comments on theoretical spectra and their culprits (Urtzi).


Are parameter values reliableAre parameter values reliable(within limits expected for a dataset of this kind)(within limits expected for a dataset of this kind)??

Just two comments from my side taken from a conferenceJust two comments from my side taken from a conferencein Palm Cove last month:in Palm Cove last month:

The library we use was extensively praised by Mike Bessell.The library we use was extensively praised by Mike Bessell. Martin Asplund's presentation had a title Martin Asplund's presentation had a title „ „Is the Sun chemically unusual?“Is the Sun chemically unusual?“


Distance fromDistance fromstellar modelsstellar models

Breddels et al. 2009, submittedBreddels et al. 2009, submitted

Distance error < 1/3 for ~1/3 of stars. Distance error < 1/3 for ~1/3 of stars.


Age Age (not published)(not published)


Improving distances fromImproving distances fromstellar modelsstellar models

Klement et al. 2008Klement et al. 2008

Currently: Currently: distance error < 1/3 for ~1/3 of stars. distance error < 1/3 for ~1/3 of stars.


RAVE starsRAVE stars

Data from Breddels et al. 2009, animation by G. MatijevičData from Breddels et al. 2009, animation by G. Matijevič

blueblue: : dwarfs (log g>3.5)dwarfs (log g>3.5)redred: : giants (log g<3.5)giants (log g<3.5)


RAVE stars (all distances we have)RAVE stars (all distances we have)

Data from Breddels (private communication), animation by G. MatijevičData from Breddels (private communication), animation by G. Matijevič



RAVE stars 220 million years agoRAVE stars 220 million years ago

Data from Breddels et al. 2009, animation G. Matijevič & M. VodopivecData from Breddels et al. 2009, animation G. Matijevič & M. Vodopivec



RAVE & RAVE & GenevaGeneva

Copenhagen Copenhagen surveysurvey

animation G. Matijevičanimation G. Matijevič

blueblue:: dwarfs (log g>3.5)dwarfs (log g>3.5)redred: : giants (log g<3.5)giants (log g<3.5)


RAVE & RAVE & SDSS SDSS surveysurvey

SDSS data by P. Re Fiorentin,SDSS data by P. Re Fiorentin,animation G. Matijevičanimation G. Matijevič



Distances in GCS, RAVE & SDSSDistances in GCS, RAVE & SDSS


Presence of Presence of giants & dwarfsgiants & dwarfs


Preclassification - scheme by Gal MatijevičPreclassification - scheme by Gal Matijevič


EyeballingEyeballing


Properties of Properties of parameters parameters

at low S/N (Corrado) at low S/N (Corrado)


Magnitude and noise distributionsMagnitude and noise distributions

For a typical giant I = 12.5corresponds to V = 13.5and g = 14.0.

Systematic errors at low S/NSystematic errors at low S/N


DR3 proposal: 3 separate catalogsDR3 proposal: 3 separate catalogs


DR4 preparationsDR4 preparations

We maintain the list of 3 catalogs Catalog A will have to be eyeballed (sic!) - August First using the new input catalog Seeking new partners – so no spectra published?

From: Sofia Feltzing <[email protected]>To: Tomaz Zwitter <[email protected]>Subject: Date: Thu, 4 Jun 2009 10:28:32 +0200X-Mailer: Apple Mail (2.753.1)

GALACTIC ASTRONOMY, GAIA AND THE NEED FOR HIGH RESOLUTION SPECTROSCOPY

A meeting at the IoA, Cambridge 8+9 July 2009---------------------------------------------


Strange things happen...Strange things happen...

Progress report on analysis and calibration of RAVE data and preparation for DR3 · 2009. 6....

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