The mass-metallicity relation and abundance gradients with KMOS 3D

Transcription

1 The mass-metallicity relation and abundance gradients with KMOS 3D Eva Wuyts, MPE E. Wisnioski, M. Fossati, N.M. Förster Schreiber, R. Genzel, D. Wilman, K. Bandara, A. Beifiori, R. Bender, G. Brammer, J. Chan, R. Davies, M. Fabricius, S. Kulkarni, P. Lang, D. Lutz, J.T. Mendel, I. Momcheva, E. Nelson, D. Rosario, R. Saglia, S. Seitz, R. Sharples, L.J. Tacconi, P. van Dokkum, S. Wuyts, et al. Understanding Nebular Emission in High-redshift Galaxies Pasadena, July 14

2 OUTLINE KMOS 3D : survey design and science goals Indicators of AGN and outflow/shock contribution to [NII] Mass-metallicity relation Effect of star formation rate Effect of environment! Abundance gradients

3 KMOS: K-band Multi-Object Spectrograph 7.2 arcmin patrol field 24 IFUs, 2.8x2.8 arcsec FOV each wavelength coverage micron R~3500 factor of 24 increase in survey speed compared to single-object IFU Sharples et al. 2004

4 Wisnioski et al KMOS 3D : Survey Design 75 nights GTO time over 5 years, started 2 years ago target Ha+[NII] for ~600 galaxies at z= quality over quantity: deep observations (4-6-8hrs in YJ-H-K) targeting southern CANDELS fields mass-selected sample with redshifts from 3D-HST

5 Wisnioski et al KMOS 3D : Survey Design 75 nights GTO time over 5 years, started 2 years ago target Ha+[NII] for ~600 galaxies at z= quality over quantity: deep observations (4-6-8hrs in YJ-H-K) targeting southern CANDELS fields mass-selected sample with redshifts from 3D-HST THE POWER OF MULTIPLEXING past surveys with single-object IFU (SINFONI and OSIRIS) over , ~300 nights of observing time for ~300 objects

6 KMOS 3D : Survey Design 75 nights GTO time over 5 years, started 2 years ago target Ha+[NII] for ~600 galaxies at z= quality over quantity: deep observations (4-6-8hrs in YJ-H-K) targeting southern CANDELS fields mass-selected sample with redshifts from 3D-HST THE POWER OF MULTIPLEXING past surveys with single-object IFU (SINFONI and OSIRIS) over , ~300 nights of observing time for ~300 objects INCREASING PARAMETER SPACE - wide redshift coverage - redder colors - probe below the main-sequence Wisnioski et al. 2015

7 KMOS 3D : Science Goals Dynamical properties - rotation-dominated versus dispersion-dominated or irregular - redshift evolution of the velocity dispersion (turbulence) - connection to stellar structure (record of past evolution)! Outflows - detect wind signatures from broad emission line components - establish ubiquity of outflows and AGN vs. star formation drivers - co-evolution with turbulence, SFR surface density,! Quenching - what causes the transition from star-forming to passive systems! Chemical Evolution - consistent study of line ratios over wide redshift range - correlations with dynamical and stellar properties - spatial variation: abundance gradients, influence of shocks/agn

8 KMOS 3D : Science Goals Dynamical properties Wisnioski et al rotation-dominated versus dispersion-dominated or irregular redshift evolution of the velocity dispersion (turbulence) connection to stellar structure (record of past evolution)! Outflows Förster Schreiber et al. 2014, Genzel et al detect wind signatures from broad emission line components establish ubiquity of outflows and AGN vs. star formation drivers co-evolution with turbulence, SFR surface density,! Quenching what causes the transition from star-forming to passive systems! Chemical Evolution consistent study of line ratios over wide redshift range correlations with dynamical and stellar properties spatial variation: abundance gradients, influence of shocks/agn

9 THE KMOS 3D SAMPLE 0.7<z< <z< <z<2.7 74% success rate 78% success rate 79% success rate

10 STANDARD ANALYSIS Wisnioski et al. 2015

11 STANDARD ANALYSIS

12 AGN and outflow/shock contribution to [NII]

13 AGN and outflow/shock contribution to [NII] [NII]/Ha > 0.6

14 AGN and outflow/shock contribution to [NII]

15 AGN and outflow/shock contribution to [NII]

16 Nuclear ionised outflows in massive SFGs Förster Schreiber et al Genzel et al. 2014

17 Nuclear ionised outflows in massive SFGs Förster Schreiber et al Genzel et al nuclear outflows FWHM ~ 1500km/s [NII]/Ha = AGN-driven

18 AGN and outflow/shock contribution to [NII]

19 AGN and outflow/shock contribution to [NII]

20 THE MASS-METALLICITY RELATION 83% detection rate of [NII]

21 THE MASS-METALLICITY RELATION 83% detection rate of [NII]

22 CORRELATION WITH STAR FORMATION RATE

23 THE EFFECT OF ENVIRONMENT Fossati et al. 2015

24 THE EFFECT OF ENVIRONMENT

25 THE EFFECT OF ENVIRONMENT

26 THE EFFECT OF ENVIRONMENT - LITERATURE Pasquali et al Peng et al. 2015

27 THE EFFECT OF ENVIRONMENT - LITERATURE Pasquali et al Peng et al. 2015

28 METALLICITY GRADIENTS

29 METALLICITY GRADIENTS TODO: fit AGN without the nuclear region

30 METALLICITY GRADIENTS

31 METALLICITY GRADIENTS 5.8sigma slope 2.9sigma without local Stott et al. 2014

32 METALLICITY GRADIENTS: A CAUTIONARY TALE Yuan et al. 2013

33 Newman+14; NMFS+15 Also, e.g., Cresci+10; Jones+10,13,15; Wright+10; Yuan+11-13; Queyrel+12; Swinbank+12; Stott+14; Troncoso+14; Shimakawa+15 And local galaxies: e.g., Zaritsky+94; Henry&Worthey99; Kewley+10; Rupke+10; Werk+11; Rich+12; Sanzhez+14; Belfiore+14 Nebular abundance gradients Typically shallow inferred metallicity gradients in z ~ 1 3 SFGs 20 massive SFGs at z ~ with well-resolved nebular metallicities on ~ 1.5 kpc scales from SINFONI+AO

34 gradient with AO METALLICITY GRADIENTS: A CAUTIONARY TALE Förster Schreiber et al., in prep. Yuan et al gradient without AO

35 METALLICITY GRADIENTS: A CAUTIONARY TALE Förster Schreiber et al., in prep. Yuan et al check effect of beam-smearing and inclination on model data! theoretical predictions for metallicity gradients from hydrodynamical simulations gradient without AO gradient with AO

36 SUMMARY!!!! KMOS3D has so far observed 420 galaxies at z= , including redder galaxies and galaxies below the MS. Overall detection rate 75-80% Removing the imprint of the galaxy kinematics on the integrated spectrum is important for accurate line width, flux and broad component measurements. The resolved data give us a unique handle on the contribution of AGN and shock ionisation from the nuclear [NII]/Ha ratio as well as broad underlying components in the nuclear spectra. We find a contribution from AGN and/or outflows for a majority of massive galaxies. [NII]/Ha is limited as an abundance indicator, but we have the first consistent measurement of a mass-selected sample over wide redshift range. We find no effect of SFR or environment on the MZR IFU data uniquely allow the measurement of abundance gradients. We need to understand the effects of beam-smearing and inclination first.!