galactic ob stars spectroscopic optical surveysiac.es/proyecto/iacob/media/sp7ewass2015/... ·...

Galactic OB stars spectroscopic optical surveys Jesús Maíz Apellániz, CAB (CSIC-INTA) La Laguna, Monday 22 June 2015

Galactic OB stars spectroscopic optical

surveys

Jesús Maíz Apellániz, CAB (CSIC-INTA)

La Laguna, Monday 22 June 2015


Talk structure1. Completed/ongoing surveys.

★ Spectroscopic, OB specific, intermediate resolution.

★ Spectroscopic, OB specific, high resolution.

★ Spectroscopic, generic.

★ Imaging + interferometry.

2. GOSSS.

3. The near future.

★ WEAVE.

★ GALANTE.


Spectroscopic, OB specific, intermediate resolution

• GOSSS: Galactic O-Star Spectroscopic Survey.

1. Completed/ongoing surveys


Spectroscopic, OB specific, high resolution


Survey PI # # O Resolution(s) Polar.? Sample Spectral types Epochs Done

OWNBarbá + Morrell 275 250 15 000 - 46 000 N S O + WN many ongoing

IACOB Simón-Díaz 525 150 23 000 - 85 000 N N O + B 3+ 90%

IACOB-sweG Negueruela 100 60 85 000 N N O + B 1 yes

NoMaDS Pellerin 120 75 30 000 N dim N O (+ B + WR) 1-few yes

CAFÉ-BEANS Negueruela 100 100 65 000 N N O ~10 80%

BOBS Chini 825 250 50 000 N S O + B ~10 ongoing

MiMeS Wade 550 100 65 000 Y all O + B + WR ~10 yes

BOB Morel 130 40 2600 - 120 000 Y S O + B few 85%


Spectroscopic, generic


1. LAMOST.

★ Northern stars down to 19th magnitude.

★ 3700-9000 Å at R from 1800 and 5000, 4000 fibers, several million stars.

★ “Survey the OB stars in the Galaxy, tracing the 3D extinction in the Galactic Plane”.

2. Gaia-RVS.

★ Whole sky down to 17th magnitude.

★ 8470-8740 Å at R ~ 11 500, ~104 O stars, many more B stars.

3. Gaia-ESO.

★ Clusters and Galactic field in the south.

★ OB stars at R ~ 20 000 but only Carina Nebula in large numbers (~800).


Why not SDSS and

RAVE?


Imaging + interferometry


Survey PI # # O Type Resolution Filters Sample Spectral types Epochs Done

Tycho-2 Høg 2.5·106 800 Im 1" BV all all many yes

IPHAS + UVEX

Drew + Groot 2.2·108 ? Im 1" Ugri+Hα

+He IN all 1-few 90%

VPHAS+ Drew 4.0·108 2000+ Im 1" Ugri+Hα S all 1-few 40%

Gaia Prusti 1.0·109 ? Prism 1" 4000 - 10 000 Å

all all many 10%

AstraLux Norte

Maíz Apellániz

900 500 LI 80 mas zi N O + B + WR 1-few yes

AstraLux Sur

Maíz Apellániz

800 400 LI 50 mas zi S O + B + WR 1 yes

SMaSH+ Sana 225 175 Interf +AO 1-30 mas HK S O 1-few 90%

Mason 561 385 Speckinterf 30 mas Vy all O + B + WR 1-few yes

FGS Gies 225 200 Interf 10 mas V all O + B 1 yes


GOSSS description

• Long-slit spectroscopy of OB stars with R~2500 and S/N > 200 in 3900-5100 Å.

• Initial selection from the Galactic O-Star Catalog (GOSC).

• Telescopes and spectrographs:★ OSN 1.5 m (Albireo): δ > −20°, B < 11★ CAHA 3.5 m (TWIN): δ > −20°, 11 < B < 14 ★ WHT 4.2 m (ISIS): δ > −20°, 11 < B < 14★ GTC 11.4 m (OSIRIS): δ > −20°, 14 < B < 17★ LCO 2.5 m (B&C): δ < −20° B < 13★ SOAR 4.1 m (GHTS): δ < −20°, 13 < B < 15★ Gemini South 8.1 m (GMOS): δ < −20°, 13 < B < 16

• 2087 stars (3390 spectra) processed (+ ~300 unproc.), compl. for B < 8.

2.GOSSS


GOSSS publications and products• Carbon lines in O stars: Walborn et al. (2010), ApJL 711, 143.

• Survey description: Maíz Apellániz et al. (2011), HSA VI, 467.

• Northern bright stars: Sota et al. (2011), ApJS 193, 24.

• Rapidly rotating ON giants: Walborn et al. (2011), AJ 142, 150.

• Specific pipeline: Sota et al. (2011), HSA VI, 785.

• MGB, spectral classification code: Maíz Apellániz et al. (2012), ASPC 465, 484.

• Southern bright stars: Sota et al. (2014), ApJS 211, 10.

• The OVz category: Arias et al. (2014), RvMxA&AC 44, 36.

• O-stars standard grid: Maíz Apellániz et al. (2015), HSA VIII.

• PhD thesis of Alfredo Sota (2015).

• Contributions to Gamen et al. (2012), A&A 546, 92; Wade et al. (2013), MNRAS 425, 1278; Salas et al. (2013), ATel 5571; Maíz Apellániz et al. (2014), IAUS 297, 117; Wade et al. (2015), MNRAS 447, 2551; Maíz Apellániz et al. (2015), A&A accepted; and Walborn et al. (2015), AJ accepted.

• Galactic O-Star Catalog (GOSC) basis: http://gosc.iaa.es .2.GOSSS

http://gosc.iaa.es


GOSSS and the other O-stars surveys• GOSSS:

★ Largest uniform sample of O stars ever (or how to clean SIMBAD).★ Spectral types (and approx. Teff + log g + v sin i).★ Intense/broad Diffuse Interstellar Bands (DIBs) in the blue-violet region (Thursday talk).★ Spatial distribution, extinction, and IMF to several kpc.★ Extreme binaries.

• Why other surveys?★ High-resolution imaging:

➡ Spatial resolution of close pairs.

★ High resolution spectroscopy: ➡ Detailed modeling: Teff + log g + v sin i + vmac + wind parameters + abundances + B field.➡ Rest of optical region: Hα, O III 5592…➡ Profile variability: intrinsic + spectroscopic binaries.➡ Weak DIBs, extension to the full optical range, atomic and molecular ISM lines.

★ Gaia: ➡ Distances.➡ Spectrophotometry.➡ Variability detection with RVS.

★ Optical imaging: ➡ New O stars.

2.GOSSS


Fundamental spectral morphology and the properties of O stars

The O-star zoo in the R~2500 GOSSS data

2.GOSSS


LS III +46 11 in Berkeley 90

2.GOSSS

0.00 0.25 0.50 0.75 1.00 1.25 1.50 1.75 2.00phase

−200

−150

−100

−50

0

50

100

150

v 1,2 (k

m/s

)

1 WHT1 HET1 CAHA−2.2 m1 NOT2 WHT2 HET2 CAHA−2.2 m 2 NOT1 fit2 fit

Hε 3

970

Hδ

4102

Hγ 4

340

Hβ

4861

He

I 400

9

He

I 412

1

He

I 414

4

He

I 416

9

He

I 438

8

He

I 443

8

He

I 447

1

He

I 471

3

He

I 492

2

He

II 42

00

He

II 45

42

He

II 46

86

He

I+II

3924

/ 27

He

I+II

4026

C II

I 406

8 / 6

9 / 7

0

C II

I 418

7

C II

I 464

7 / 5

0 / 5

1C

IV 4

658

N II

I 409

7

N II

I 437

9

N II

I 451

1 / 1

5

N II

I 463

4 / 4

1 / 4

2

N II

I 490

5

N IV

405

8

N V

460

4 / 2

0

Si IV

408

9

Si IV

411

6

Si IV

463

1

Si IV

465

4

DIB

is 4

179

DIB

is 4

428

DIB

is 4

502

DIB

is 4

591

DIB

is 4

727

DIB

is 4

761

/ 62

DIB

is 4

780

DIB

is 4

880

/ 87

Ca

II is

393

4

Ca

II is

396

8

CH

is 4

300

CH

+ is

423

2C

a I i

s 42

27

LS III +46 11 O3.5 If* + O3.5 If*

LS III +46 11 O3.5 If* + O3.5 If*

LS III +46 12 O4.5 V((f))

4000 4250 4500 4750Wavelength (Å)

0.50

0.75

1.00

1.25

1.50

1.75

2.00

20:35:05

20:35:10

20:35:15

20:35:20

20:35:25

20:35:30

+46:49:00

+46:50:00

+46:51:00

+46:52:00

+46:53:00

LS III + 46 11

LS III + 46 12

2MASS J20350798+4649321


WEAVE: the instrument

• Double-arm optical Multi-Object Spectrograph for the 4.2 m WHT.

• ~950 fibers (+20 mIFUs and 1 LIFU).

• 2 degrees diameter FOV.

• Low resolution mode (R~5000): 3700 - 10 000 Å.

• High resolution (R~20 000).

• Survey-oriented.

3. The near future


WEAVE: Galactic Plane Stellar, Circumstellar, and Interstellar Physics

• OBA-stars-centered survey that plans to get ~10% of WEAVE survey time.

• Also ISM in emission, Cepheids, evolved low-mass stars, and other young stars.

• R ~ 5000, whole optical range.

• Galactic Plane with longitudes from 20 deg. to 225 deg.

• 1200 sq. deg.

• 2-3·105 targets.3. The near future

0 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15B

ap magnitude

1

3

10

30

100

300

1000

Num

ber

Confirmed O stars

40 O stars/kpc2, 0.8 mag/kpc





Why GALANTE?

• Some problems with photometric surveys for OB stars:

★ Saturation.

★ Filter selection.

★ Footprint.

★ Field of view and old instrumentation.

★ Long-term instrument stability and repeatability.

3. The near future


Javalambre: observatory and projects

• New observatory in Teruel, Spain.

• CEFCA: Centro de Estudios de Física del Cosmos de Aragón.

• Two telescopes: T250 and T80.

• Exclusive for wide-field optical imaging surveys.

• T80:

★ 1.4 deg x 1.4 deg.

★ 9216x9232 px, 0.55”/px.

★ In commissioning.

★ Low read-out noise, up to 0.1” exposures.

3. The near future


T80 images

3. The near future


The GALANTE survey

• Northern Galactic Plane.

• ~3 nights/month in the T80.

• Exposure times from 0.1 to 10 s.

★ Saturation ~ mag 6.

★ S/N ~ 100 at mag 16.

• Six filters:

★ F348M + F4220N + F450N.

★ F515N.

★ F660N + F665N.3. The near future

F348M F420N F450N

3250 3500 3750 4000 4250 4500 4750Wavelength (Å)

0.00

0.25

0.50

0.75

1.00

1.25

1.50

F λ/F

λ(400

0 Å)

7 000 K 10 000 K 15 000 K 20 000 K 30 000 K 50 000 K


The GALANTE survey





★ S/N ~ 100 at mag 16.

• Six filters:

★ F348M + F4220N + F450N.

★ F515N.


−1.5 −1.0 −0.5 0.0 0.5 1.0 1.5 2.0F348M−3.44F420N+2.44F450N

0.00

0.25

0.50

0.75

1.00

F420

N−1

.47F

450N

+0.4

7F51

5N

MW MS E(4405−5495) = 0.0 R5495

= 3.1

Teff

= 4,7,10,15,20,30,50 kK


The GALANTE survey





★ S/N ~ 100 at mag 16.

• Six filters:

★ F348M + F4220N + F450N.

★ F515N.


−1.5 −1.0 −0.5 0.0 0.5 1.0 1.5 2.0F348M−3.44F420N+2.44F450N

0.00

0.25

0.50

0.75

1.00

F420

N−1

.47F

450N

+0.4

7F51

5N

MW MS E(4405−5495) = 0.0 R5495

= 3.1

MW SG E(4405−5495) = 0.0 R5495

= 3.1

Teff

= 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK


The GALANTE survey





★ S/N ~ 100 at mag 16.

• Six filters:

★ F348M + F4220N + F450N.

★ F515N.


−1.5 −1.0 −0.5 0.0 0.5 1.0 1.5 2.0F348M−3.44F420N+2.44F450N

0.00

0.25

0.50

0.75

1.00

F420

N−1

.47F

450N

+0.4

7F51

5N

MW MS E(4405−5495) = 0.0 R5495

= 3.1

MW SG E(4405−5495) = 0.0 R5495

= 3.1

SMC MS E(4405−5495) = 0.0 R5495

= 3.1

Teff

= 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK


The GALANTE survey





★ S/N ~ 100 at mag 16.

• Six filters:

★ F348M + F4220N + F450N.

★ F515N.


−1.5 −1.0 −0.5 0.0 0.5 1.0 1.5 2.0F348M−3.44F420N+2.44F450N

0.00

0.25

0.50

0.75

1.00

F420

N−1

.47F

450N

+0.4

7F51

5N

MW MS E(4405−5495) = 0.0 R5495

= 3.1

MW SG E(4405−5495) = 0.0 R5495

= 3.1

SMC MS E(4405−5495) = 0.0 R5495

= 3.1

MW MS E(4405−5495) = 1.0 R5495

= 3.1

Teff

= 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK


The GALANTE survey





★ S/N ~ 100 at mag 16.

• Six filters:

★ F348M + F4220N + F450N.

★ F515N.


−1.5 −1.0 −0.5 0.0 0.5 1.0 1.5 2.0F348M−3.44F420N+2.44F450N

0.00

0.25

0.50

0.75

1.00

F420

N−1

.47F

450N

+0.4

7F51

5N

MW MS E(4405−5495) = 0.0 R5495

= 3.1MW SG E(4405−5495) = 0.0 R

5495 = 3.1

SMC MS E(4405−5495) = 0.0 R5495

= 3.1MW MS E(4405−5495) = 1.0 R

5495 = 3.1

MW MS E(4405−5495) = 1.0 R5495

= 5.0T

eff = 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK T

eff = 4,7,10,15,20,30,50 kK

Teff

= 4,7,10,15,20,30,50 kK T

eff = 4,7,10,15,20,30,50 kK


The GALANTE survey

• Main objectives:

★ Identify all OB stars and all Hα excess stars in the Northern Galactic Plane down to magnitude 16.

★ Estimate Teff for the sample above.

★ Measure E(4405-5495) and R5495 for the OBA stars in the sample by cross-matching with 2MASS.

• Sample additional objectives:

★ Detect previously unidentified high proper-motion stars.

★ Obtain a homogeneous sample of Ae/Be stars.


The GALANTE survey

• Possible extensions:

★ Deep surveys of interesting regions.

★ The time domain.

★ Beyond the Galactic Plane: Orion, M31, M33…

★ Additional filters: Ca triplet window, Na I D1+D2, TiO…

★ Twin telescope in the South.

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