Ionized gas properties in local galaxies SANTIAGO ERROZ-FERRER - - PowerPoint PPT Presentation

The MUSE Atlas of Disks (MAD)

SANTIAGO ERROZ-FERRER

Marcella Carollo, Mark den Brok, Masato Onodera, Victor Debattista

• R. Bacon, J. Brinchmann, T. Contini, E. Emsellem, B.Guiderdoni, D. Krajnovic, S. Lilly, R. Marino, J.

Schaye, L. Wisotzki, Anna Cibinel, Sandro Tacchella, Joanna Woo and the GTO-MUSE Team

Ionized gas properties in local galaxies

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

Ionized gas properties at <100 pc scales

Erroz-Ferrer et al. (in prep)

Number of Voronoi cells Median = 26 pc ~500000 cells

2D maps of gas diagnostics derived from strong emission lines

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

New BPT parameter: η

P1 P2 P3

η<#0.5 η>0.5 #0.5<η<0.5

SF AGN/. shock

η

BPT parameter

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

Ionized gas properties at <100 pc scales 2D maps of gas diagnostics derived from strong emission lines

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch ➡ MASS-METALLICITY RELATION AT 0.5 Re FOR ALL STRUCTURES! ➡ EMPIRICAL CALIBRATIONS SATURATE

Calibrations with different nature:

• 1. Empirical calibrations using HII regions, e.g., Marino et al. 2013 (M13)
• 2. Photoionzation models, e.g., Dopita et al. 2016 (DOP16)

Gas metallicity inside 0.5 Re

• We adopt the calibration in Dopita et al. 2016 as fiducial (can be used for regions

with hard radiation fields)

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

Gas metallicity gradients

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

➡ Using Dopita calibration eliminates rising gradients ➡ Declining and flat metallicity gradients: centers of

disks always more metal rich than outskirts

➡ Gradient is similar for SF & AGN/Shocked-gas! ➡ Gradient is similar for HII & DIG! ➡ Gradient does not change with stellar mass

Gradients Gas metallicity gradients: summary ALL DIG SF gas HII

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

• Slope flattens with increasing total mass
• At fixed Σ*, the higher the total stellar mass, the higher the metallicity
• We find resolved mass-metallicity relation, holds at ~100 pc scales
• Slope flattens at ~103 M⊙pc-2

log[Σ*/M⊙pc-2] Resolved mass-metallicity relation 12+log(O/H) Trends with total mass

—> LOCAL METAL ENRICHMENT DEPENDS OF GLOBAL POTENTIAL AND/OR PAST SFH

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

Secondary relations? Colour-code by a third quantity Trends with SFR?

• SFR suggested to be a second

parameter in the M-Z relation (e.g., Manucci+10)

• MaNGA & CALIFA do not find this

relation at local scales (Barrera- Ballesteros+2017, Sánchez+2017)

• Little evidence for the local SFR

density to act as a second- parameter

Resolved mass-metallicity relation

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

Trends with SFR? HII regions Diffuse Ionized Gas

Holds for both HII & DIG gas!

Resolved mass-metallicity relation

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

• Slope increases with increasing total mass, but not significantly
• Similar range of ΣSFR at all mass bins. Local dependence?

log[Σ*/M⊙pc-2] Trends with total mass log[ΣSFR/M⊙yr-1kpc-2]

• Mass-SFR holds at low- and high-z: Star Formation Main Sequence
• We find a correlation at ~100 pc scales, but with scatter

Resolved mass-SFR relation

— HII — DIG

• Relation only holds when considering both HII and DIG regions

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch

Secondary relations? Trends with metallicity?

• Only relation between Σ* and

metallicity

• Metallicity increases with total Mass

Resolved mass-SFR relation

Malta 2017 Santiago Erroz-Ferrer serrozfe@phys.ethz.ch The MUSE ATLAS OF DISKS (MAD) program probes local star-forming disks on <<100pc scales, enabling us: → to disentangle HII begins from AGN/shock gas and Diffuse Ionised Gas (DIG) → to to study the impact of AGN/shock gas and Diffuse Ionised Gas (DIG)

• n SFR and gas (kinematics and) metallicities
• The DIG has often a lower Zgas but a very similar Zgas-gradient than the HII regions
• A suitable choice of Zgas CALIBRATION is crucial:

→ Outward-rising Zgas-gradients are in most cases an artefact of a saturation in Zgas calibration → Secular inward gas flow typically brings highly-enriched star-formation fuel to the inner bulge regions

• A “local mass-metallicity” relation exists down to the <<100pc scales of MAD, but, on such

scales, we see little evidence for the local SFR density to act as a second-parameter

• The local SFR density depends on the local stellar mass density, but the local metal enrichment

depends on the total stellar mass (i.e., SFH and/or gravitational potential)

CONCLUSIONS

Ionized gas properties in z=0 galaxies at <100 pc scales