Galactic OB stars spectroscopic optical surveys

Transcription

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

2 Talk structure 1. 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.

3 Spectroscopic, OB specific, intermediate resolution GOSSS: Galactic O-Star Spectroscopic Survey. 1. Completed/ongoing surveys

4 Spectroscopic, OB specific, high resolution Survey PI # # O Resolution(s) Polar.? Sample Spectral types Epochs Done OWN Barbá + Morrell N S O + WN many ongoing IACOB Simón-Díaz N N O + B 3+ 90% IACOB-sweG Negueruela N N O + B 1 yes NoMaDS Pellerin N dim N O (+ B + WR) 1-few yes CAFÉ-BEANS Negueruela N N O ~10 80% BOBS Chini N S O + B ~10 ongoing MiMeS Wade Y all O + B + WR ~10 yes BOB Morel Y S O + B few 85% 1. Completed/ongoing surveys

5 Spectroscopic, generic 1. LAMOST. Northern stars down to 19th magnitude 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 Å at R ~ , ~10 4 O stars, many more B stars. 3. Gaia-ESO. Clusters and Galactic field in the south. OB stars at R ~ but only Carina Nebula in large numbers (~800). 1. Completed/ongoing surveys

6 Galactic OB stars spectroscopic optical surveys Why not SDSS and RAVE? Jesús Maíz Apellániz, CAB (CSIC-INTA) La Laguna, Monday 22 June 2015

7 Imaging + interferometry Survey PI # # O Type Resolution Filters Sample Spectral types Epochs Done Tycho-2 Høg Im 1" BV all all many yes IPHAS + UVEX Drew + Groot ? Im 1" Ugri+Hα +He I N all 1-few 90% VPHAS+ Drew Im 1" Ugri+Hα S all 1-few 40% Gaia Prusti ? Prism 1" AstraLux Norte AstraLux Sur Maíz Apellániz Maíz Apellániz SMaSH+ Sana Å all all many 10% LI 80 mas zi N O + B + WR 1-few yes LI 50 mas zi S O + B + WR 1 yes Mason Interf +AO Speck interf 1-30 mas HK S O 1-few 90% 30 mas Vy all O + B + WR 1-few yes FGS Gies Interf 10 mas V all O + B 1 yes 1. Completed/ongoing surveys

8 GOSSS description Long-slit spectroscopy of OB stars with R~2500 and S/N > 200 in 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 < stars (3390 spectra) processed (+ ~300 unproc.), compl. for B < 8. 2.GOSSS

9 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: 2.GOSSS

10 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

11 Fundamental spectral morphology and the properties of O stars The O-star zoo in the R~2500 GOSSS data 2.GOSSS

12 20:35:30 20:35:25 20:35:20 20:35:15 20:35:10 20:35: He I+II 3924 / 27 Ca II is 3934 Ca II is 3968 He I 4009 He I+II 4026 N IV 4058 C III 4068 / 69 / 70 N III 4097 He I 4121 He I 4144 He I 4169 C III 4187 He II 4200 CH + is 4232 CH is 4300 LS III O3.5 If* + O3.5 If* N III 4379 He I 4388 He I 4438 He I 4471 N III 4511 / 15 He II 4542 N V 4604 / 20 N III 4634 / 41 / 42 C III 4647 / 50 / 51 C IV 4658 He II 4686 He I 4713 N III 4905 He I 4922 LS III in Berkeley :53: :52:00 LS III O3.5 If* + O3.5 If* 1.25 LS III :51: LS III O4.5 V((f)) :50:00 LS III Hε 3970 Si IV 4089 Hδ 4102 Si IV 4116 DIB is 4179 Ca I is 4227 Hγ 4340 DIB is 4428 DIB is 4502 DIB is 4591 Si IV 4631 Si IV 4654 DIB is 4727 DIB is 4761 / 62 DIB is 4780 Hβ 4861 DIB is 4880 / 87 2MASS J :49:00 Wavelength (Å) WHT 1 HET 1 CAHA 2.2 m 1 NOT 2 WHT 2 HET 2 CAHA 2.2 m 2 NOT 1 fit 2 fit v 1,2 (km/s) phase 2.GOSSS

13 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): Å. High resolution (R~20 000). Survey-oriented. 3. The near future

14 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. Number Confirmed O stars 40 O stars/kpc 2, 0.8 mag/kpc 30 O stars/kpc 2, 0.6 mag/kpc 15 O stars/kpc 2, 0.4 mag/kpc 8 O stars/kpc 2, 0.2 mag/kpc sq. deg targets. B ap magnitude 3. The near future

15 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

16 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

17 T80 images 3. The near future

18 T80 images 3. The near future

19 T80 images 3. The near future

20 T80 images 3. The near future

21 The GALANTE survey Northern Galactic Plane. ~3 nights/month in the T80. Exposure times from 0.1 to 10 s K K K K K K Saturation ~ mag 6. S/N ~ 100 at mag 16. Six filters: F348M + F4220N + F450N. F λ /F λ (4000 Å) F515N. F660N + F665N F348M F420N F450N Wavelength (Å) 3. The near future

22 The GALANTE survey Northern Galactic Plane. ~3 nights/month in the T80. Exposure times from 0.1 to 10 s MW MS E( ) = 0.0 R 5495 = 3.1 Saturation ~ mag 6. S/N ~ 100 at mag 16. Six filters: F348M + F4220N + F450N. F515N. F660N + F665N. F420N 1.47F450N+0.47F515N F348M 3.44F420N+2.44F450N 3. The near future

23 The GALANTE survey Northern Galactic Plane. ~3 nights/month in the T80. Exposure times from 0.1 to 10 s MW MS E( ) = 0.0 R 5495 = 3.1 MW SG E( ) = 0.0 R 5495 = 3.1 Saturation ~ mag 6. S/N ~ 100 at mag 16. Six filters: F348M + F4220N + F450N. F515N. F660N + F665N. F420N 1.47F450N+0.47F515N F348M 3.44F420N+2.44F450N 3. The near future

24 The GALANTE survey Northern Galactic Plane. ~3 nights/month in the T80. Exposure times from 0.1 to 10 s MW MS E( ) = 0.0 R 5495 = 3.1 MW SG E( ) = 0.0 R 5495 = 3.1 SMC MS E( ) = 0.0 R 5495 = 3.1 Saturation ~ mag 6. S/N ~ 100 at mag 16. Six filters: F420N 1.47F450N+0.47F515N F348M + F4220N + F450N. F515N. F660N + F665N F348M 3.44F420N+2.44F450N 3. The near future

25 The GALANTE survey Northern Galactic Plane. ~3 nights/month in the T80. Exposure times from 0.1 to 10 s MW MS E( ) = 0.0 R 5495 = 3.1 MW SG E( ) = 0.0 R 5495 = 3.1 SMC MS E( ) = 0.0 R 5495 = 3.1 MW MS E( ) = 1.0 R 5495 = 3.1 Saturation ~ mag 6. S/N ~ 100 at mag 16. Six filters: F420N 1.47F450N+0.47F515N F348M + F4220N + F450N. F515N. F660N + F665N F348M 3.44F420N+2.44F450N 3. The near future

26 The GALANTE survey Northern Galactic Plane. ~3 nights/month in the T80. Exposure times from 0.1 to 10 s MW MS E( ) = 0.0 R 5495 = 3.1 MW SG E( ) = 0.0 R 5495 = 3.1 SMC MS E( ) = 0.0 R 5495 = 3.1 MW MS E( ) = 1.0 R 5495 = 3.1 MW MS E( ) = 1.0 R 5495 = 5.0 Saturation ~ mag 6. S/N ~ 100 at mag 16. Six filters: F420N 1.47F450N+0.47F515N F348M + F4220N + F450N. F515N. F660N + F665N F348M 3.44F420N+2.44F450N 3. The near future

27 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( ) 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.

28 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.