Automated Fitting Automated Fitting of High-Resolution of High-Resolution Spectra of HAeBe Spectra of HAeBe

starsstarsImproving fundamental Improving fundamental parametersparameters

Jason GrunhutJason GrunhutQueen’s University/RMCQueen’s University/RMC

MotivationMotivation Common ways to Common ways to

determine temperaturedetermine temperature PhotometryPhotometry SEDSED

ProblemsProblems Extinction/emission and Extinction/emission and

calibrationscalibrations Many corrections necessaryMany corrections necessary

Take advantage of high-res Take advantage of high-res ESPaDOnS spectraESPaDOnS spectra Minimal corrections requiredMinimal corrections required

Full ESPaDOnS Spectral Range Full ESPaDOnS Spectral Range 11000 K synthetic model11000 K synthetic model

Full ESPaDOnS Spectral Range Full ESPaDOnS Spectral Range 11000 K synthetic model11000 K synthetic model

Spectrum variation with temperature Spectrum variation with temperature from nearest Kurucz models (from nearest Kurucz models (±500 K)±500 K)

Spectrum variation with temperature Spectrum variation with temperature from nearest Kurucz models (from nearest Kurucz models (±500 K)±500 K)

Automated Fitting of Automated Fitting of SpectraSpectra

Search through a pre-defined grid of Search through a pre-defined grid of synthetic spectra.synthetic spectra. 4200-5200 Angstroms4200-5200 Angstroms Solar abundances.Solar abundances. Most current VALD line list.Most current VALD line list. Micro-turbulent velocity of 2 km/s.Micro-turbulent velocity of 2 km/s. No macro-turbulence.No macro-turbulence. Models computed using synth3Models computed using synth3 Grid from 6500-35000 K, log(g) from Grid from 6500-35000 K, log(g) from

3.0-5.03.0-5.0 100 K resolution up to 20000 K, 200 K 100 K resolution up to 20000 K, 200 K

resolution from then up.resolution from then up.

How Program WorksHow Program Works

Radial velocity is first determined Radial velocity is first determined based on suggested model.based on suggested model.

Projected rotational velocity is fit for Projected rotational velocity is fit for each model in the specified range each model in the specified range (computed using slightly modified (computed using slightly modified s3dIV code).s3dIV code).

Model with minimum chi-square Model with minimum chi-square represents best fit.represents best fit.

Radial velocity is fit for a final time Radial velocity is fit for a final time for best model.for best model.

Theoretical Results for Theoretical Results for 11000 K synthetic model 11000 K synthetic model

with vsini of with vsini of 40 km/s40 km/s

CLEAR MINIMUM

EXISTS

Chi-Square MapChi-Square MapHD 17081HD 17081

• Using chi-square map, can estimate uncertainties.

• Using 3 parameter fitting space, chi-square difference of 21.1 represents a formal 99.99% confidence level.

• closest model has greater than 2300 chi-square difference

Theoretical ResultsTheoretical Results

• Investigated

• SNR

• vsini

• varying Fe abundance

• random noise to log(gf) values

• micro/macro turbulence

• binaries

• normalization

• conclusion

• other than binaries, for reasonable variations, ~100-200 K uncertainties

ResultsResultsNameName Metallic Metallic

LinesLines(Teff, (Teff,

Log(g))Log(g))

ReducReduced ed χχ22

HHγγ(Teff, Log(g))(Teff, Log(g))

HHββ(Teff, (Teff,

Log(g))Log(g))

Literature Literature

ValueValue

HD HD 142666142666

7700, 4.07700, 4.0 6.686.68 7300, 3.57300, 3.5 7500, 4.57500, 4.5 85008500

HD HD 144432144432

7700, 4.07700, 4.0 7.167.16 7200, 3.07200, 3.0 7400, 4.57400, 4.5 79507950

HD 17081HD 17081 13700, 13700, 4.04.0

6.216.21 11800, 3.511800, 3.5 12000, 12000, 4.04.0

1230012300

HD HD 244604244604

8600, 3.58600, 3.5 5.295.29 8200, 4.08200, 4.0 8100, 4.08100, 4.0 ~9500~9500

HD 31648HD 31648 8200, 3.58200, 3.5 25.7725.77 8300, 4.08300, 4.0 8300, 4.08300, 4.0 8700 8700 ± ± 10051005

HD 34282HD 34282 10200, 10200, 4.54.5

2.232.23 9800, 4.59800, 4.5 10100, 10100, 4.54.5

8700 8700 +410/-198+410/-198

HD 35187HD 35187 9200, 4.09200, 4.0 4.664.66 8700, 4.08700, 4.0 8600, 4.08600, 4.0 9100 9100 ± ± 420420

HD 36112HD 36112 7900, 4.07900, 4.0 5.365.36 8000, 5.08000, 5.0 8100, 5.08100, 5.0 7750 7750 ± ± 358358

HD 53367HD 53367 31200, 31200, 4.54.5

3.613.61 29200, 4.029200, 4.0 31400, 31400, 4.04.0

31600 31600 ± ± 36503650

HD 17081HD 17081

• B7IV Classification

•Best Fit

• 13700 K

• Log(g)=4.0

• vsini=20 km/s

• Literature Results

• ~12300 K

HD 17081HD 17081

HD 17081HD 17081

HD 17081 Balmer FitsHD 17081 Balmer Fits

Best Fit: 11800 K, Log(g)=3.5

Best Fit: 12000 K, Log(g)=4.0

HD 34282HD 34282

• A0e+sh Classification

• Best Fit

• 10200 K

• Log(g)=4.5

• vsini=108 km/s

•Literature Results

• ~8700 (+410,-198) K

HD 34282HD 34282

HD 34282 Balmer FitsHD 34282 Balmer Fits

Best Fit: 9800 K, Log(g)=4.5

Best Fit: 10100 K, Log(g)=4.5

HD 36112HD 36112

• A8e Classification

• Best Fit

• 7900 K

• Log(g)=4.0

• vsini=52 km/s

• Literature Results

• ~7700 K

HD 36112HD 36112

HD 36112 Balmer FitsHD 36112 Balmer Fits

Best Fit: 8000 K, Log(g)=5.0

Best Fit: 8100 K, Log(g)=5.0

HD 31648HD 31648

• A3pshe+ Classification

• Best Fit

• 8200 K

• Log(g)=3.5

• vsini=95 km/s

• Literature Results

• 8700 K

• 9250 K, Log(g)=3.5

HD 31648HD 31648

Difficult Stars:Difficult Stars:BF OriBF Ori

• A5II-IIIe var

• Best Fit

• ~7500

• Log(g)~4.0

• vsini~53 km/s

• Literature Results

• 6750

BF OriBF Ori

HR DIAGRAM:HR DIAGRAM:New TemperaturesNew Temperatures

HR Diagram:HR Diagram:New Temperatures and New Temperatures and

DistancesDistances

HR Diagram:HR Diagram:New Temperatures and New Temperatures and Computed PhotometryComputed Photometry

FUTURE WORKFUTURE WORK Automated fitting for all field HAeBe stars Automated fitting for all field HAeBe stars

with ESPaDOnS observations.with ESPaDOnS observations. Use improved temperatures to improve Use improved temperatures to improve

mass and age estimates.mass and age estimates. Use Bayesian statistical approach to Use Bayesian statistical approach to

improving luminosities.improving luminosities.Major IssuesMajor Issues

Abundances for chemically peculiar stars.Abundances for chemically peculiar stars. Micro/macro turbulence.Micro/macro turbulence. Systematic normalization issues.Systematic normalization issues.

THE ENDTHE END

Balmer Line Normalization: Balmer Line Normalization: HD36112HD36112

Balmer Line Normalization: Balmer Line Normalization: HD139614HD139614

Balmer Line Normalization:Balmer Line Normalization:Comparison between ESPaDOnS Comparison between ESPaDOnS

and FORS1and FORS1HD 36112

Uncertainty vs SNRUncertainty vs SNRFor 15000 K synthetic model with 40 For 15000 K synthetic model with 40

km/s vsini.km/s vsini.

15000 K synthetic model 15000 K synthetic model with with

40 km/s vsini40 km/s vsini

Difficult stars:Difficult stars:HD 31293HD 31293

HD 31293HD 31293