Multiconjugate Fluctuations: Measuring SBF with GeMS

Transcription

1 Multiconjugate Fluctuations: Measuring SBF with GeMS John Blakeslee (NRC Herzberg, Victoria) & Joe Jensen (UVU) Gemini Science Meeting 18 June 2015

2 HST/WFC3 F160W IC3032

3 HST/WFC3 F160W

4 S/N

5 SBF in the 90s: Ground-based I-band survey of ~300 galaxies (Tonry et al. 1997, 2000, 2001 Blakeslee et al. 1999, 2002) SBF distances used to constrain peculiar veloci3es, Virgo infall; H 0 = 74 ± 6 km/s/mpc βi = 0.44 ± 0.05 Ω m 0.25 (Blakeslee, Davis, Tonry et al. 1999) Data from: MDM, CTIO, KPNO, LCO, CFHT, WFPC2 Median error of 0.22 mag, ~ 10% in d.

6 SBF fluctuation magnitude versus (g-z) color: composite stellar population VRIz predictions bright z-band SBF bright; predicted scatter ~0.06 mag. Blakeslee, Vazdekis, & Ajhar (2001) composite models. Other SBF models: Worthey 1993 Liu et al Cantiello et al Raimondo+ 2005, 2009 Marin-Franch & Apparicio 2006 Lee et al red

7 Virgo in 3-D ACS Virgo Cluster Survey Mei, Blakeslee, Cote+ 2007

8 SBF Results from ACS Fornax + Virgo Surveys Fornax cluster 21±1% more distant than Virgo cluster. intrinsic scatter σ = 0.06 mag Blakeslee, Jordan, Mei+ 2009

9 Multiple Type Ia SNe in NGC 1316 Can6ello et al. 2013

10 Tonry et al SBF catalog s6ll the most widely used d s for local E galaxy BH & kinema6c studies (e.g., ATLAS- 3D) ~d ~d ~d 2 ~d 0

11 The MASSIVE Sample: targeting high-mass galaxies requires larger distances MASSIVE survey N4889 ATLAS 3d survey M87 Ma et al. 2014

12 Infrared SBF l SBF is ~30 more luminous at K than at I Dominated by luminous RGB stars l Increased contrast with (less contamination from) globular clusters & background galaxies l Seeing is better in the near-ir l Extinction is much lower than in the optical l Sensitive to young populations and AGB stars l Age-metallicity degeneracy is broken à IR SBF can reach greater distances à IR SBF can reveal young and intermediate components in unresolved stellar populations

13 Preliminary WFC3/IR SBF Calibrations Fornax Virgo E de/s0 Jensen, Blakeslee et al (arxiv: )

14 F814-F160W SBF color vs V-I IMF?

15 SBF with Multi-conjugate AO? , 0.02 /pix, 2 arcmin 2 FOV 3 deformable mirrors; 5 laser guide stars; 3 natural tip-tilt stars Uniform 0.08 PSF across But issues with variable distortion.

16 Ferrarese+ 2007, WFPC2 Cepheid distance

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22 J K

23 ESO

24 ESO

25 ESO

26 Summary & Outlook With < 5% errors per galaxy, SBF has become most complete and precise distance indicator in the d = Mpc range; provides precise distances to hundreds of local E- types, reveals structure of Virgo; enables important tests of SN Ia. Excellent agreement of theore6cal and empirical SBF zero points; best H 0 = 72.9 ± 4.3 km/s/mpc from Coma cluster. WFC3/IR SBF now calibrated; very efficient for studies of velocity field, black hole scaling rela6ons, stellar pops, etc. Pilot SBF study w/gems GSAOI promising: beder resolu6on than WFC3/IR plus K- band capability, but s0ll ba3ling the spa0al PSF varia0ons & temporal varia0on in distor0on. Looking forward to NGS 2 and new laser!

27 The End

28 The MASSIVE Survey Combine wide-field and high-resolution (AO) IFUs Wide field (107 x107 ) Mitchell IFU McDonald 2.7m 256 fibers each å Out to ~2 Re for >50% galaxies High-resolution (~0.1 to 3 ) OSIRIS + AO Keck NIFS + AO Gemini GMOS N+S Gemini Photometry HST, NIRC2, PanSTARRS C.-P. Ma (Berkeley) & Jenny Greene (Princeton) Nicholas McConnell (IfA)

29 The MASSIVE Sample (PI s: C-P Ma & Jenny Greene) F-J Relation N4889 MASSIVE M87 ATLAS 3d Ma et al. 2014

30 Under-explored parameter space at high mass; requires targeting galaxies at larger distances MASSIVE survey N4889 ATLAS 3d survey M87 Ma et al. 2014

31 HST SBF vs MLCS SNIa (H0=74) (Ajhar et al. 2001) Caution: SNIa & SBF from Pre-ACS/WFC3 era: use for historical purposes only.

32 SBF stellar pop models: support for Cepheid zero point NGC 1316 Teramo SPoT stellar population models (Raimondo et al 2005, 2009). Empirical & model SBF zero point calibrations agree within 0.05 mag.

33 Multiple Type Ia SNe in NGC 1316

34 SN Ia Distances to NGC 1316 NGC 1316 SN Ia Jha, Riess & Kirshner 2007 Stritzinger etal Tripp Stritzinger et al NIR 1980N ± ± ± D ± ± ± dd ± ± mr ± ± % SBF-SNIa discrepancy for NGC1316 (see Cantiello et al. 2013)

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36 SBF Distances to NGC 1316 Tonry et al ground I-band, V-I calib ± 0.17 Cantiello et al ACS I814, V555-I814 calib ± 0.08 JPB et al ACS z850, g475-z850 calib ± 0.07 JPB et al Cantiello et al ACS I814, g475-i814 calib V,I,z,J,H ACS+WFC3+VLT ± ± 0.05

37 The 3-D Structure of Virgo: Velocity-distance relation Mei, Blakeslee, Cote et al. 2007

38 3-D Structure of Virgo Mean error per galaxy: σ (m-m) = 0.07 mag, or 0.5 Mpc. Triaxial structure, with axial ratios about 1 : 0.7 : 0.5 Line-of-sight depth of main cluster = 2.4±0.4 Mpc (i.e., ±2σ intrinsic distribution). Spatial distribution of dwarfs follows that of giants. Group of galaxies associated with NGC 4365 (W Cloud) about 6.5 Mpc behind main cluster; infalling at ~ 450 km/s. Other substructure evident, e.g., the high-velocity galaxy M86 (NGC4406) and companions ~ 1 Mpc beyond the core. M87 and M49 subclusters at same d 16.5 Mpc.

39 M87 HST image, before & after galaxy model subtraction