the shape of oxygen abundance profiles explored with muse...conclusions oxygen abundance gradients...
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The shape of oxygen abundance profiles explored with MUSE
Sebastián F. Sánchez –IA/UNAM
- Cosmic feast of elements - Puebla (MX), 2017
The shape of oxygen abundance profiles explored with MUSE
Sebastián F. Sánchez –IA/UNAM
- Cosmic feast of elements - Puebla (MX), 2017
http://adsabs.harvard.edu/abs/2017arXiv171001188S
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
Spiral galaxies present gradients in the color, luminosity, Ha flux density and EW(Ha) reflecting a differential evolution from the inner to the outer parts: inside-out scenario (80's, 90's).Since Smith (1973) and Peimbert et al. (1977) , it is known that Hii regions in Sc/Sd galaxies present a negative abundance gradient: Chemical enrichment happens faster in the inner parts.Systematic search were hampered by the number of spectra to be taken: e.g., Vila Costas et al. 1992, Martin et al. 1994...Several individual studies (Bresolin, Pilyugin, Rosales Ortega... since 90's).What we learn from large IFU surveys?
Abundance gradients: Historical results
CALIFA: Common abundance gradient
Sánchez et al., A&A Sánchez et al., A&A 2013,2014a2013,2014a
FWHM ~ 0.7 kpc
Gradients determined at 0.3<R/Re<2.1.207 galaxias, ~6500 regions 9000 Hii reg.→Gradients distribution compatibles with a single Gaussian function.Slope ~ -0.11+-0.08 dex/Reff.
CALIFA: Common abundance gradientFWHM ~ 0.7 kpc
300 galaxies (nHii>4)
Sanchez et al. 2014, A&A, 563, 49
CALIFA: Common abundance gradientFWHM ~ 0.7 kpc
300 galaxies (nHii>4)
CALIFA: Common abundance gradientFWHM ~ 0.7 kpc
Sanchez-Menguiano,2016, A&A, 587, 70
Mass
CALIFA: Common abundance gradient
Common gradient
flatenning
drop
FWHM ~ 0.7 kpc
MaNGA: Common abundance gradient?Belfiore et al. 2017, MNRAS, 469, 151FWHM ~ 3 kpc
Fitted range Fitted range
CALIFA vs. MaNGA: abundance gradientSánchez & Sánchez-Menguiano, 2017, RMxAA, 49, 28FWHM ~ 0.7 kpc ~3 kpc
CALIFA
CALIFA
MaNGA, Re>2.5”
MaNGA, Re>2.5”
Is a resolution effect?Mast et al., 2014, A&A, 561, 129
The HubbleSequenceObserved By MUSE
Top: B,R,I colourimage,showing the stelllar populations.
Bottom: [OIII] (B),Ha (G), [NII] (R ),showing the ionized gas.
Elliptical S0 Sa Sb
Sc Sd
Int./Irregular
MUSE@VLT:FoV = 1'x1', 0.2”/spaxel, 90,000 spectra, R~3000, 4650-9300 AA AMUSING survey (PI: J.Anderson) + Archive: ~350 galaxias
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
102 Spiral galaxies.0.005<z<0.07 <z>~0.015.Good coverage of the blue cloud.All spiral morphological types.Very similar to SM16.
z g-r
Mabs,r (mag)
Pipe3D: An IFU anaysis pipeline for MaNGA, CALIFA, SAMI, and MUSE
Broad-band + S/N Central Aperture+FIT3D+small SSP template (6 SSPs)+Strong Em. lines
- Sys. Vel.- σcen
- Range of param.
RSS+FIT3D+small SSP template (12 miuscat SSPs 3600-9500 AA)
+Strong Em. Lines
- St. Vel. map.- St. σ map.- St. Av map.(Cardielli et al. 1998, curve)
Datacube
Gas pure Datacube →Analysis of the strong and weak emission lines
Gas “cleaned” datacubeRSS-segmented
FIT3D+large SSP template (156 SSPs 3600-7200 AA)SFH, Age, [Z/H], St. Mass
Sanchez et al., 2016, RMxAA, 52, 171
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
http://www.astroscu.unam.mx/~sfsanchez/HII_explorer/
# HII regions ~ 14,000
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Neighbourhood Presence of Bars Shape of the profile
Typical profile of ~ -0.1 dex/Re Does not depends on (I)
environment, (II) presence of
bars, or (III) stellar Mass. Mass range shorter than
Belfiore et al. 2017
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Inner drop ~0.5 R/Re. Outer flatenning ~ 1.5 R/Re New scale-length in galaxies, RO/H: distance at which scale drops 0.1 dex (Pilyugin et al.). RO/H ~ Re Common gradient.→ Inner drop = 0.5 R/RO/H Outer flatenning = 1.5 R/RO/H
R/Re
R/RO/H
log(R/RO/H)
log(R/Re)
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Inner drop is present at higher masses (Sánchez-Menguiano et al. 2016; Belfiore et al. 2017; Sánchez et al. 2017) Flatenning seems to be universal (?).
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Main results do not depend on the O/H calibrator Common gradient. Location of Inner and Outer drop.
The inner drop is less or more evident depending on the calibrator
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Main results do not depend on the O/H calibrator Common gradient. Location of Inner and Outer drop.
The inner drop is less or more evident depending on the calibrator
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Inner drop is present at higher masses (Sánchez-Menguiano et al. 2016; Belfiore et al. 2017; Sánchez et al. 2017) Flatenning seems to be universal (?).
MUSE CALIFA
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
The MW seems to follow a similar trend, but...(1) The Re is very badly characterize.... thus slope ~ -0.15 dex/Re.(2) We do not see the flatenning (so far?)(3) Inner drop is just hinted.
MUSE +MW (Estaban et al. 2017)
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
AMUSING++ : Shape of the O/H gradient FWHM ~ 0.2 kpc
Dispersion around the main radial distribution does not depends on galaxy properties: Implications on radial/azimuthal migration?
Sanchez-Menguiano et al., A&A, in press (arXiv:1710.01188)
Conclusions Oxygen abundance gradients in spiral galaxies seem to
present three range: (a) common-gradient (~-0.1 dex), (b) inner drop (~0.5 Re), (c) outer-flatenning (~1.5Re).
Common-gradient is confirm between 109.5 – 1012 Msun. Abundance gradients becomes shallower at << 108.5
Msun. Resolution may have a strong impact in the analysis of
abundance gradients of FWHM > 1kpc. Galaxy properties (beyond interaction) do not seem
to have a strong effect in the shape of the profile. Little influence of radial or azimuthal migrations (?).
O/H enrichment seem to be govern by local processes: (a) inside-out differential SFH (Perez et al. 2013); (b) central quenching (or outlflows?); (c) outer migration/change of abundance efficient.