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Exploring the Local Group massive star content with 2-4m telescopes at ORM and CAHA

Exploring the Local Group massive star content with 2-4m telescopes at ORM and CAHA. S. Simón-Díaz (IAC) on behalf of the IAC (PI. A. Herrero) CAB/CSIC (PI. F. Najarro) UA (PI. I. Negueruela) IAA/CSIC (J. Maíz Apellániz) massive star groups + M. Garcia, A. Marco, J. Lorenzo, A. Sota.

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Exploring the Local Group massive star content with 2-4m telescopes at ORM and CAHA

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  1. Exploring the Local Group massive star content with 2-4m telescopes at ORM and CAHA S. Simón-Díaz (IAC) on behalf of the IAC (PI. A. Herrero) CAB/CSIC (PI. F. Najarro) UA (PI. I. Negueruela) IAA/CSIC (J. Maíz Apellániz) massive star groups + M. Garcia, A. Marco, J. Lorenzo, A. Sota ... Science with the optical-infrared telescopes at CAHA and ORM in the coming decade Madrid, 2012 March 22nd

  2. Exploring the Local Group massive star content Things we are doing / plan to do using optical* telescopes at CAHA and ORM Milky Way • The GOSSS project • spectral types • catalogue • atlas • binaries + Detailed studies of selected candidates + Detailed study of binaries + Detect and characterize OB associations • The IACOB project • vsini / macrot. • stellar/wind parameters • abundances • binaries • time-dependent phenomena • + IACOB-sweG * For the infrared part see Ignacio Negueruela’s talk (just after me)

  3. Exploring the Local Group massive star content Things we are doing / plan to do using optical* telescopes at CAHA and ORM Local Group galaxies (other than the MW) • Detect luminous blue stars • (B Sgs, O stars, LBV, WRs) • Characterize OB associations • Spectral types • Stellar & wind parameters • Abundances in a evolutionary context • 1D/2D abundance distributions • Detailed studies of selected candidates M31 M33 * For the infrared part see Ignacio Negueruela’s talk (just after me)

  4. Exploring the Local Group massive star content (optical spectroscopy) What can we do depending of the characteristics of the spectra? Resolving power R: > 15000 8000-10000 5000 2000-3000 Spectral types: More than enough ok ok ok Stellar/wind param.: Perfect feasible feasible at limit Abundances: Optimal good feasible at limit vsini_min (km/s) < 20 30-40 60 100-150 Binary detection < 7 km/s ~10 km/s ~20 km/s ~40 km/s ** Nebular (HII spectrum) contamination **

  5. Exploring the Local Group massive star content (optical spectroscopy) What can we do depending of the characteristics of the spectra? Signal-to-noise ratio SNR/pixel: > 150 100-150 50-100 < 50 Spectral types: More than enough ok ok too bad Stellar/wind param.: Perfect good at limit too bad Abundances: Optimal good at limit too bad vsini Optimal possible at limit too bad

  6. Exploring the Local Group massive star content (optical spectroscopy) What can we do depending of the characteristics of the spectra? Spectral range coverage 3700 – 7000 A : Optimal 4000 – 4700 A : Minimum requirement for spectral types 4000 – 5000 A + Ha : Minimum requirement for quantitative spectroscopy (stellar & wind parameters + abundances) SiIII 4552 & OIII 5591 : very important lines for vsini (B & O-type stars)

  7. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Telescopes/instruments • The GOSSS project(PI. Maiz Apellaniz) • The Galactic O star spectroscopic survey aims at being complete up to B < 13 • ~1500 stars * Spectral types • R ~ 2500 • SNR ~ 300 • 3900 – 5100 A * Binary detection  Multi-epoch 2007 - xxx OSN - 1.5m CAHA - 3.5m ISIS@WHT - 4.2m Long-slit spectroscopy Future ~ 50% of the survey is still missing – depends of TAC decission in next semesters

  8. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Telescopes/instruments • The IACOB project(PI. Simón-Díaz) • * Line-broadening in OB stars • * Quantitative spectroscopic analyses • * Abundances in OB-type stars • * Massive binary/multiple systems • R > 20000 • SNR > 200 • 3900 – 7000 A • Multi-epoch • IACOB survey: Northern OB-type stars • with V<8  ~200 stars 2008 – 2012? FIES@NOT - 2.5m R =23000, 46000 (3900-7000 A) Future ~ 98% of the survey is complete but a couple of observing runs (2x4 nights) will allow to increase the number of detected binaries  NOT future !!! + HERMES@MERCATOR - 1.2m + CAFE@CAHA - 2.2m

  9. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Telescopes/instruments • The IACOB project(PI. Simón-Díaz) • * Line-broadening in OB stars • * Quantitative spectroscopic analyses • * Abundances in OB-type stars • * Massive binary/multiple systems • R > 20000 • SNR > 200 • 3900 – 7000 A • Multi-epoch • IACOB survey: Northern OB-type stars • with V<8  ~200 stars 2008 – 2012? FIES@NOT - 2.5m HERMES@MERCATOR - 1.2m Future Requires long time-series observations Observing campaings of ~ 1-2 weeks per semester during several years Also CAFE@CAHA - 2.2m ??

  10. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Telescopes/instruments • IACOB-sweG(PI. Negueruela) • IACOB supplemented with an extension to the Gaia spectral range • Grid of Galactic standards • SpT: O4 – B9 • LC: V, IV, III, II, Ib, Iab, Ia • R > 20000 • SNR > 100 • 3900 – 9000 A 2010-2012 HERMES@MERCATOR - 1.2m R =85000 (3900-9000 A) Future ~ 50% of the survey is complete (due to bad weather)  New proposal (4 nights) this semester

  11. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Telescopes/instruments • + Detailed studies of massive binaries • previously detected by GOSSS & IACOB • R > 8000 (but better if R>15000) • SNR > 100 • Multi-epoch (periods from a few hours to years) IDS@INT - 2.5m ISIS@WHT - 4.2m FIES@NOT - 2.5m HERMES@MERCATOR - 1.2m Future CAFÉ-BEANS (PI. Negueruela) Proposal submitted recently to the CAHA guaranteed time CAFE@CAHA - 2.2m

  12. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Telescopes/instruments • + Detect and characterize OB associations • (including metallicity via B-type stars) • R > 8000 • SNR > 100 • 4000 - 5000 A (+Ha) • Combined with wide-field imagery (OB associations) WFC@INT - 2.5m IDS@INT - 2.5m ISIS@WHT - 4.2m FIES@NOT - 2.5m HERMES@MERCATOR - 1.2m CAFE@CAHA - 2.2m Future Spectroscopic follow up for Gaia blue massive stars in (reddened) OB associations in the Milky Way with WEAVE@WHT

  13. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Spectroscopic follow-up for GAIA blue massive stars • - We will use WEAVE to obtain spectra of all the members of Galactic OB associations. • * The brightest members are already spectroscopically confirmed OB stars, for which high resolution spectroscopy and quantitative analysis is already underway. • * But Gaia will unveil new reddened members, for which it will provide approximate spectroscopic classification and accurate distance measurements • * Nearby Milky Way OB associations typically extend 1 squared degree across the sky (see seminal catalogs by Humphreys or Massey) • Example: Cas OB6 and Aur OB2 have a population of ~400 and 800 candidate blue massive star (Massey et al. (1995)) with V between 8 and 18. • Good quality high resolution spectra for all the brightest members can be achieved with one single WEAVE pointing. • - Gaia will undoubtfully add new OB stars and association candidates to current lists. Notes provided by Miriam Garcia (IAC)

  14. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Milky Way Spectroscopic follow-up for GAIA blue massive stars An example provided by Artemio Herrero (IAC) • Massey & Tompson (1991) classify 70 OB stars in Cyg OB2 • Based on 2MASS photometry, Knödlseder (2000) suggests that Cyg OB contains over 100 O stars (not just OB) • Comeron et al. (2002) downsize it to 90-100 O stars and Hanson (2003) confirms Comeron et al. findings observing the brightest stars between B = 12.0 - 14.5 • Negueruela et al. (2008) find new O stars and evidence for differet ages or aletrnative evolutionary scenarios

  15. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Local Group galaxies (other than the MW) • B-Sgs as tracers of abundance gradients • Luminous stellar objects • But not bright enough to be observed at high-resolution • 4m-class telescopes are needed  WHT4.2m • R – texp – SNR + spectral range coverage compromise Typical configuration: ISIS 1.2 arcsec slit R1200B and R1200R (R~5000, 3900-4800 A + Ha) SNR=80 for V=17.5 star (3 x 3600s) Seeing < 1.0 Grey moon 2-3 stars per night !!!! Thanks to the dicroic

  16. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Local Group galaxies (other than the MW) B-Sgs as tracers of abundance gradients (how things were done in the past) Good science case ... ... but very inefficient instrumental configuration + needs already discovered candidates From Urbaneja et al. (2005) Dots: HII regions from Vilchez et al. (1988)

  17. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Local Group galaxies (other than the MW) B-Sgs as tracers of 2D abundance distributions (how we do things now) 1 deg M33

  18. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Local Group galaxies (other than the MW) B-Sgs as tracers of 2D abundance distributions (how we do things now) • WFC@INT (U,B,V) 33x33 arcmin • > First selection of candidates (using appropiate photometric indicators) • > Accurate astrometry • AF2/WYFFOS@WHT • > 20 arcmin effective diameter • > 80-100 effective fibers (1.6 arcsec) • > R1200B + R1200R (R=2500) • > 4000 – 5000 A + Ha • > 8.5h: SNR=40 (V=18), 75 (V=17) • > Confirmation of candidates • > B-Sgs: 2D abundance distribution 1 deg M33

  19. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Local Group galaxies (other than the MW) But not only B-Sgs as tracers of 2D abundance distributions + Detect luminous blue stars (B Sgs, O stars, LBV, WRs) + Characterize OB associations + Spectral types ** OK with WFC + R=2500 ** + Stellar & wind parameters + Abundances in a evolutionary context + 1D/2D abundance distributions + Detailed studies of selected candidates OK to a first order, but ** better if higher resolution **

  20. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Local Group galaxies (other than the MW) How things could improve in the near future: WEAVE@WHT AF2/WYFFOS@WHT > 2 degrees FoV > 800-1000 fibers (1.2 – 1.5 arcsec) > R=5000 > 4000 – 9000 A AF2/WYFFOS@WHT > 20 arcmin effective diameter > 80-100 effective fibers (1.6 arcsec) > R1200B + R1200R (R=2500) > 4000 – 5000 A + Ha > 8.5h: SNR=40 (V=18), 75 (V=17)

  21. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Massive stars in Local Group galaxies: science case for WEAVE Resolved massive stars in Local Group galaxies: Complete census of the unreddened massive star content in the Local Group. Some notes by M. Garcia & A. Herrero (IAC) • We want to get spectral classifications for all massive star candidates in Northern Local Group galaxies up to V= 19.0 • The resulting spectral types will be used for studies of global populations and to design follow up spectroscopic studies with larger telescopes for the most interesting cases: • The quantitative spectroscopic analysis of a comprehensive sample of massive stars across the Local Group will allow us to study their physics, evolution, winds and feedback as a function of environment. • Massive stars can be used as tracers of metallicity.

  22. Exploring the Local Group massive star content Science with the optical telescopes at CAHA & ORM Conclusions • We can do many things regarding massive star in the Milky Way and other Local Group galaxies using optical facilities at CAHA and ORM • Specially remarcable is the importance of the high-resolution spectrographs (+efficient pipelines) attached to 1-4m telescopes for the detailed studies of bright Galactic OB stars. Less pressure  more chances to get time for the binary and variability projects (+ large surveys) • Multi-object spectroscopy is really valuable for us (as for many other science cases), and WEAVE will be of great benefit for the study of massive star in the Milky Way and other Local Group Galaxies.

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