Milky Way analogues in MaNGA: multiparameter homogeneity and comparison to the Milky Way

Boardman, Nicholas Fraser; Zasowski, Gail; Seth, Anil; Newman, Jeffrey A.; Andrews, Brett H.; Bershady, Matthew A.; Bird, Jonathan C.; Chiappini, Cristina; Fielder, Catherine E.; Fraser-McKelvie, Amelia; Jones, Amy; Licquia, Timothy C.; Masters, Karen L.; Minchev, Ivan; Schiavon, Ricardo P.; Brownstein, Joel R.; Drory, Niv

doi:10.1093/mnras/stz3126

Cited by 31 publications

(20 citation statements)

References 176 publications

(218 reference statements)

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“…Another interesting feature seen in Fig. 4 is the differences in inner slope exhibited by different SL diagnostics for massive galaxies (see also Boardman et al 2020b). Those diagnostics which rely on [O ] lines (i.e.…”

Section: Metallicity Diagnosticsmentioning

confidence: 83%

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Yates

Henriques

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a modified version of the L-Galaxies 2020 semi-analytic model of galaxy evolution, which includes significantly increased direct metal enrichment of the circumgalactic medium (CGM) by supernovae (SNe). These more metal-rich outflows do not require increased mass-loading factors, in contrast to some other galaxy evolution models. This modified L-Galaxies 2020 model is able to simultaneously reproduce the gas-phase metallicity (Zg) and stellar metallicity (Z*) radial profiles observed in nearby disc galaxies by MaNGA and MUSE, as well as the observed mass – metallicity relations for gas and stars at z = 0 and their evolution back to z ∼ 2 − 3. A direct CGM enrichment fraction of ∼90 per cent for SNe-II is preferred. We find that massive disc galaxies have slightly flatter Zg profiles than their lower-mass counterparts in L-Galaxies 2020, due to more efficient enrichment of their outskirts via inside-out growth and metal-rich accretion. Such a weak, positive correlation between stellar mass and Zg profile slope is also seen in our MaNGA-DR15 sample of 571 star-forming disc galaxies, although below ${\rm log}_{10}{(M_{*}/{\rm M_\odot} )}{}\sim {}10.0$ this observational result is strongly dependent on the metallicity diagnostic and morphological selection chosen. In addition, a lowered maximum SN-II progenitor mass of 25 M⊙, reflecting recent theoretical and observational estimates, can also provide a good match to observed Zg and Z* profiles at z = 0 in L-Galaxies 2020. However, this model version fails to reproduce an evolution in Zg at fixed mass over cosmic time, or the magnesium abundances observed in the intracluster medium (ICM).

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Section: Metallicity Diagnosticsmentioning

confidence: 83%

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Yates

Henriques

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…To analyze the present-day AVR of h277, we wish to define a region that is solar neighborhood-like. Boardman et al (2020) showed that the scatter in radial gradients of MW analogues is minimized if galaxies are normalized by disk scale length, R d . The best-fit exponential profile to the disk-dominated (R > 2.5 kpc) stellar surface mass density yields R d = 2.42 kpc.…”

Section: Results: the Present-day Avrmentioning

confidence: 99%

“…Here, rather than adopt a fix radius to define the solar neighborhood, we have scaled the solar neighborhood based on the relative difference in scale length R d of the simulated disk compared to the MW. Boardman et al (2020) showed that the scatter in various radial properties of disk galaxies is minimized when scaling by R d , suggesting that this scaling is the best way to directly compare to the MW's AVR.…”

Section: Other Factors That Impact Heating Resultsmentioning

confidence: 99%

Inside Out and Upside-Down: The Roles of Gas Cooling and Dynamical Heating in Shaping the Stellar Age-Velocity Relation

Bird,

Loebman,

Weinberg

et al. 2020

Preprint

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Kinematic studies of disk galaxies, using individual stars in the Milky Way or statistical studies of global disk kinematics over time, provide insight into how disks form and evolve. We use a high-resolution, cosmological zoom-simulation of a Milky Way-mass disk galaxy (h277) to tie together local disk kinematics and the evolution of the disk over time. The present-day stellar age-velocity relationship (AVR) of h277 is nearly identical to that of the analogous solar-neighborhood measurement in the Milky Way. A crucial element of this success is the simulation's dynamically cold multi-phase ISM, which allows young stars to form with a low velocity dispersion (σ birth ∼ 6 − 8 km s −1 ) at late times. Older stars are born kinematically hotter (i.e., the disk settles over time in an "upside-down" formation scenario), and are subsequently heated after birth. The disk also grows "inside-out", and many of the older stars in the solar neighborhood at z = 0 are present because of radial mixing. We demonstrate that the evolution of σ birth in h277 can be explained by the same model used to describe the general decrease in velocity dispersion observed in disk galaxies from z ∼ 2 − 3 to the present-day, in which the disk evolves in quasi-stable equilibrium and the ISM velocity dispersion decreases over time due to a decreasing gas fraction. Thus, our results tie together local observations of the Milky Way's AVR with observed kinematics of high z disk galaxies.

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“…As a whole, the radial gradients in our simulations are somewhat steeper than in external galaxies but somewhat shallower than in the MW. The MW may be an outlier: as Boardman et al (2020) note, its gradient is typically steeper than those observed in MW analogs. These differences are likely the result of a combination of different factors, such as: measuring over different radial ranges or using different calibrators.…”

Section: Radial Profiles At Z =mentioning

confidence: 98%

3D gas-phase elemental abundances across the formation histories of Milky Way-mass galaxies in the FIRE simulations: initial conditions for chemical tagging

Bellardini

Wetzel

Loebman

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We use FIRE-2 simulations to examine 3-D variations of gas-phase elemental abundances of [O/H], [Fe/H], and [N/H] in 11 MW and M31-mass galaxies across their formation histories at z ≤ 1.5 ($t_{\rm lookback} \le 9.4 \, \rm {Gyr}$), motivated by characterizing the initial conditions of stars for chemical tagging. Gas within $1 \, \rm {kpc}$ of the disk midplane is vertically homogeneous to $\lesssim 0.008 \, \rm {dex}$ at all z ≤ 1.5. We find negative radial gradients (metallicity decreases with galactocentric radius) at all times, which steepen over time from $\approx -0.01 \, \rm {dex}\, \rm {kpc}^{-1}$ at z = 1 ($t_{\rm lookback} = 7.8 \, \rm {Gyr}$) to $\approx -0.03 \, \rm {dex}\, \rm {kpc}^{-1}$ at z = 0, and which broadly agree with observations of the MW, M31, and nearby MW/M31-mass galaxies. Azimuthal variations at fixed radius are typically $0.14 \, \rm {dex}$ at z = 1, reducing to $0.05 \, \rm {dex}$ at z = 0. Thus, over time radial gradients become steeper while azimuthal variations become weaker (more homogeneous). As a result, azimuthal variations were larger than radial variations at z ≳ 0.8 ($t_{\rm lookback} \gtrsim 6.9 \, \rm {Gyr}$). Furthermore, elemental abundances are measurably homogeneous (to ≲ 0.05 dex) across a radial range of $\Delta R \approx 3.5 \, \rm {kpc}$ at z ≳ 1 and $\Delta R \approx 1.7 \, \rm {kpc}$ at z = 0. We also measure full distributions of elemental abundances, finding typically negatively skewed normal distributions at z ≳ 1 that evolve to typically Gaussian distributions by z = 0. Our results on gas abundances inform the initial conditions for stars, including the spatial and temporal scales for applying chemical tagging to understand stellar birth in the MW.

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Milky Way analogues in MaNGA: multiparameter homogeneity and comparison to the Milky Way

Cited by 31 publications

References 176 publications

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

L-GALAXIES 2020: The evolution of radial metallicity profiles and global metallicities in disc galaxies

Inside Out and Upside-Down: The Roles of Gas Cooling and Dynamical Heating in Shaping the Stellar Age-Velocity Relation

3D gas-phase elemental abundances across the formation histories of Milky Way-mass galaxies in the FIRE simulations: initial conditions for chemical tagging

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