1 / 32

Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO

Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO. Martin Bureau, Oxford University. SAURON (R. Bacon, M. Cappellari, R.L. Davies, E. Emsellem, J. Falcon-Barroso, D. Krajnovic, M. Sarzi, H. Kuntschner, R.M. McDermid, R.F. Peletier, G. van de Ven, P.T. de Zeeuw) CO

zwi
Download Presentation

Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO Martin Bureau,Oxford University SAURON (R. Bacon, M. Cappellari, R.L. Davies, E. Emsellem, J. Falcon-Barroso, D. Krajnovic, M. Sarzi, H. Kuntschner, R.M. McDermid, R.F. Peletier, G. van de Ven, P.T. de Zeeuw) CO (A. Crocker, F. Combes, L.M. Young) GALEX (H. Jeong, Y-K. Sheen, S.K. Yi) Plans:Optical/SAURON: Stellar populations in E/S0s and KDCs CO/BIMA:Star formation material, accretion, HI UV/GALEX:Current and recent star formation Summary

  2. Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO Martin Bureau,Oxford University SAURON (R. Bacon, M. Cappellari, R.L. Davies, E. Emsellem, J. Falcon-Barroso, D. Krajnovic, M. Sarzi, H. Kuntschner, R.M. McDermid, R.F. Peletier, G. van de Ven, P.T. de Zeeuw) CO (A. Crocker, F. Combes, L.M. Young) GALEX (H. Jeong, Y-K. Sheen, S.K. Yi) Plans:Optical/SAURON: Stellar populations in E/S0s and KDCs CO/BIMA: Star formation material, accretion, HI UV/GALEX: Current and recent star formation Summary

  3. Galaxy Formation Goals: • Mass assembly history (galaxies vs. stars) • Chemical enrichment history Context: • Hierarchical structure formation (merging, harassment, ...) • Subsequent dynamical evolution (BH/triaxiality-driven, ...) ⇒ Exploit "fossil record" (near-field cosmology) (Juneau et al 05)

  4. SAURON: Stellar Linestrengths(Kuntschner et al. 06, 08) Main results: • Standard: Homogeneously old, decreasing metallicity (larger spread among S0s) • Occasional: Young core/body, increasing metallicity • Isoindices: Mgb isoindex countours often flatter than light (40%; rotators)

  5. Stellar Pop.: Classic KDCs(McDermid et al. 06) Classic KDCs: • Large: kpc's(0.3-0.4 Re) • Massive • Coeval: homogeneously old • Non-rotators Formation: • Early (dissipative) major merging, then quiescent? • Recent dissipationless major merging (dry mergers)? SAURON Data:

  6. Stellar Pop.: Compact KDCs(McDermid et al. 06) SAURON-OASIS Data: Compact KDCs: • Small: 100 pc's(≤ 0.1 Re) • Lightweight • Young: distinct, younger toward center (contrary to ionized gas) • Rotators Formation: • Recent dissipative minor merging/accretion?

  7. KDCs: Age-Size Dichotomy(McDermid et al. 06) SAURON-OASIS Data: Central pixel Compact KDCs: • Small: 100 pc's(≤ 0.1 Re) • Lightweight • Young: distinct, increasingly young toward center • Rotators Classic KDCs: • Large: kpc's(0.3-0.4 Re) • Massive • Coeval: homogeneously old • Non-rotators

  8. Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO Martin Bureau,Oxford University SAURON (R. Bacon, M. Cappellari, R.L. Davies, E. Emsellem, J. Falcon-Barroso, D. Krajnovic, M. Sarzi, H. Kuntschner, R.M. McDermid, R.F. Peletier, G. van de Ven, P.T. de Zeeuw) CO (A. Crocker, F. Combes, L.M. Young) GALEX (H. Jeong, Y-K. Sheen, S.K. Yi) Plans:Optical/SAURON: Stellar populations in E/S0s and KDCs CO/BIMA:Star formation material, accretion, HI UV/GALEX: Current and recent star formation Summary

  9. CO: Single-Dish Survey(Combes, Young & Bureau 07) IRAM 30m Survey: • CO(1-0), 23” FWHM (2-1), 12” FWHM • 39/48 SAURON E/SOs • Sensitivity: 2-4 mK (30 km s-1) 1-5 x 107 M⊙ • Literature results Results: • 28% detection rate (12/43) • As expected for L, type • <CO(2-1)/CO(1-0)> ≈ 1.4 High S/N: Low S/N:

  10. CO: Dust, FIR, SF(Combes, Young & Bureau 07) Correlations: • MH2 – FIR correlation (and normalised) • Extension of Kennicutt-Schmidt relation • High SFE

  11. CO: L, Linestrengths, SF(Combes, Young & Bureau 07) Correlations: • More CO for ...  Low type, L, σ  High Hβ, low Fe and Mg  High Hα, low B-V, age • Trends appear ultimately “driven” by SF • Confirmed by FIR/radio continuum ratio

  12. CO: Central Disks(Young, Bureau & Cappellari 08; Bureau & Young, in prep) Central Disks: • CO cospatial with young stars and central stellar/gas disk • CO and stars/gas co-rotating CRs: • CO roughly cospatial with young stars and CR/gas (generally less extended) • CO and stars/gas kinematics unrelated ? (triggered SF?) BIMA-SAURON Data: NGC4526 DSS+CO “age” Hβ CO SAURON V★+CO VCO

  13. CO: Central Disks(Young, Bureau & Cappellari 08; Bureau & Young, in prep) Central Disks: • CO cospatial with young stars and central stellar/gas disk • CO and stars/gas co-rotating CRs: • CO roughly cospatial with young stars and CR/gas (generally less extended) • CO and stars/gas kinematics unrelated ? (triggered SF?) BIMA-SAURON Data: NGC4459 DSS+CO “age” Hβ SAURON CO VCO V★+CO

  14. CO: Central Disks(Young, Bureau & Cappellari 08; Bureau & Young, in prep) Central Disks: • CO cospatial with young stars and central stellar/gas disk • CO and stars/gas co-rotating CRs: • CO roughly cospatial with young stars and CR/gas (generally less extended) • CO and stars/gas kinematics unrelated ? (triggered SF?) BIMA-SAURON Data: NGC3032 DSS+CO “age” Hβ SAURON CO V★+CO VCO

  15. CO: Central Disks(Young, Bureau & Cappellari 08; Bureau & Young, in prep) Central Disks: • CO cospatial with young stars and central stellar/gas disk • CO and stars/gas co-rotating CRs: • CO roughly cospatial with young stars and CR/gas (generally less extended) • CO and stars/gas kinematics unrelated ? (triggered SF?) BIMA-SAURON Data: NGC4150 DSS+CO “age” Hβ CO SAURON V★ VCO

  16. CO: NGC2768 (PdB)(Crocker, Bureau, Young & Combes, 08) CO(1-0): CO vs. SAURON: • CO in a centrally-concentrated rotationally-supported polar disk (rotates like ionised gas) • CO traces dip in (stellar) σ • CO traces Hβ (SF) gas • No evidence of young stars! ICO VCO CO(2-1): ICO VCO

  17. CO: NGC2768 (PdB)(Crocker, Bureau, Young & Combes, 08) SAURON EW([OIII]): SAURON EW(Hβ): CO vs. SAURON: • CO in a centrally-concentrated rotationally-supported polar disk (rotates like ionised gas) • CO traces Hβ(SF) gas • CO traces dip in (stellar)σ • No evidence of young stars! EW(Hβ)+ICO σ★+ICO SAURON Hβ abs.: SAURON Hβ/[OIII]: Hβ abs. [OIII]/Hβ+ICO

  18. CO: External Accretion HI: NGC2685, NGC2768: • Generic accretion model for polar rings (although likely a polar disk) Generally: • Disturbed HI (Morganti et al. 06) • Lack of strong correlations CO-optical (e.g. scale, L, ...) • Many galaxies with CO but no HI! (Morganti et al. 06) CO:

  19. Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO Martin Bureau,Oxford University SAURON (R. Bacon, M. Cappellari, R.L. Davies, E. Emsellem, J. Falcon-Barroso, D. Krajnovic, M. Sarzi, H. Kuntschner, R.M. McDermid, R.F. Peletier, G. van de Ven, P.T. de Zeeuw) CO (A. Crocker, F. Combes, L.M. Young) GALEX (H. Jeong, Y-K. Sheen, S.K. Yi) Plans:Optical/SAURON: Stellar populations in E/S0s and KDCs CO/BIMA: Star formation material, accretion, HI UV/GALEX:Current and recent star formation Summary

  20. GALEX: UV Upturn(Jeong et al., in prep) UV Upturn: Normal:

  21. NGC2974: UV Morphology - Kin.(Jeong et al. 07) Optical-UV Imaging: Distribution: • Young stars and RSF (UV bright and blue) in centre + outer ring • Possible larger partial ring Barred Dynamics: • [OIII] nuclear and inner rings • Imply unique pattern speed  Bar-driven SF (single pattern speed)

  22. NGC2974: UV Morphology - Kin.(Jeong et al. 07) Optical-UV Imaging: Distribution: • Young stars and RSF (UV bright and blue) in centre + outer ring • Possible larger partial ring Barred Dynamics: • [OIII] nuclear and inner rings • Imply unique pattern speed  Bar-driven SF (single pattern speed) Log (EW[OIII]) Resonances

  23. NGC2974: Stellar Pop. Modeling(Jeong et al. 07) NUV-V FUV-V χ2 fit SED Age YC χ2 fit Fraction YC SED

  24. Other Cases: NGC2273(Jeong et al., in prep) GALEX-MDM: HI Hα (Noordermeer et al. 05)

  25. Other Cases: NGC2273(Jeong et al., in prep) V GALEX-MDM: I VHβ Hβ UM [OIII]/Hβ (Falcon-Barroso et al. 06)

  26. Other Cases: NGC2273(Jeong et al., in prep) V OVRO CO: I CO VHβ σHβ [OIII]/Hβ (Petitpas & Wilson 02) (Falcon-Barroso et al. 06)

  27. Other Cases: NGC4274(Jeong et al., in prep) GALEX-MDM: ICO VCO (Noordermeer et al. 05) (Koda et al. 05)

  28. Other Cases: NGC4274(Jeong et al., in prep) SAURON: ICO V σ σHβ VHβ VCO (Noordermeer et al. 05) [OIII]/Hβ [OIII]/Hβ (Koda et al. 05) (Falcon-Barroso et al. 06)

  29. Other Cases: NGC5953(Jeong et al., in prep) SAURON: VHI HI (Iono et al. 05) CO VCO (Noordermeer et al. 05) VCO CO

  30. Gas Accretion and SF in Nearby Early-Types: UV, Optical, CO Martin Bureau,Oxford University SAURON (R. Bacon, M. Cappellari, R.L. Davies, E. Emsellem, J. Falcon-Barroso, D. Krajnovic, M. Sarzi, H. Kuntschner, R.M. McDermid, R.F. Peletier, G. van de Ven, P.T. de Zeeuw) CO (A. Crocker, F. Combes, L.M. Young) GALEX (H. Jeong, Y-K. Sheen, S.K. Yi) Plans:Optical/SAURON: Stellar populations in E/S0s and KDCs CO/BIMA: Star formation material, accretion, HI UV/GALEX: Current and recent star formation Summary

  31. (Preliminary) Conclusions • KDCs: - Classic KDCs: Large, massive, homogeneously old, non-rotator (early dissipational/late dissipationless major merger) - Compact KDCs: Small, lightweight, young, rotator (minor merger/gas accretion) • CO: - Central disks:CO cospatial/corotating with gas/young stars - Central CRs:CO roughly cospatial with gas/young stars (generally less extended), unrelated to CRs ? ✗ Still in exploratory phase, building up sample... • UV: - Resolved UV-optical colors:Constraints on age, mass fraction, and surface density of young stars - Recent SF correlated with dynamics (disk formation ?) (both secular and externally-triggered SF) ✗ Statistical and UV-upturn analyses to come...

  32. Conclusions: Future Atlas3D: • Complete volume-limited E/SO sample: - 257 E/S0s within ≈ 40 Mpc (and visible from La Palma; ≈ 200 new targets) - 38 guaranteed nights on WHT (>70 objects done in 14 nights April) - 115 hours on IRAM 30m so far... (sample already 75% complete; ≥20% detection rate, no significant cluster-field difference) ✗Also obtaining optical IFU data for E/S0s with existing CO maps...

More Related