The Leoncino Dwarf Galaxy: Exploring the Low-metallicity End of the Luminosity–Metallicity and Mass–Metallicity Relations*

McQuinn, Kristen B. W.; Berg, Danielle A.; Skillman, Evan D.; Adams, Elizabeth A. K.; Cannon, John; Dolphin, Andrew E.; Salzer, John J.; Giovanelli, Riccardo; Haynes, Martha P.; Hirschauer, Alec S.; Janoweicki, Steven; Klapkowski, M.; Rhode, Katherine L.

doi:10.3847/1538-4357/ab7447

Cited by 39 publications

(57 citation statements)

References 98 publications

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“…It has been determined, however, that the scatter in the mass-metallicity is lower than the scatter in the luminosity-metallicity relation (Berg et al 2012), an indication that it is stellar mass that is more fundamentally linked than luminosity to a galaxy's metallicity. The gas-phase mass-metallicity relation (MZR), has since been studied in great detail for dwarf galaxies (Lequeux et al 1979;López-Sánchez 2010;Berg et al 2012;Calabrò et al 2017;McQuinn et al 2020), large statistical samples of galaxies (Tremonti et al 2004;Lara-López, López-Sánchez & Hopkins 2013c;Curti et al 2020), E-mail: sabine.bellstedt@uwa.edu.au galaxies that fall below the MZR (Peeples, Pogge & Stanek 2009), and integral field data (Sánchez et al 2013(Sánchez et al , 2019a, etc. to understand why this relation exists, and what its implications are for galaxy evolution.…”

Section: Introductionmentioning

confidence: 99%

Galaxy and mass assembly (GAMA): the inferred mass–metallicity relation from z = 0 to 3.5 via forensic SED fitting

Bellstedt

Robotham

Driver

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We analyse the metallicity histories of ∼4,500 galaxies from the GAMA survey at z < 0.06 modelled by the SED-fitting code ProSpect using an evolving metallicity implementation. These metallicity histories, in combination with the associated star formation histories, allow us to analyse the inferred gas-phase mass–metallicity relation. Furthermore, we extract the mass–metallicity relation at a sequence of epochs in cosmic history, to track the evolving mass–metallicity relation with time. Through comparison with observations of gas-phase metallicity over a large range of redshifts, we show that, remarkably, our forensic SED analysis has produced an evolving mass–metallicity relationship that is consistent with observations at all epochs. We additionally analyse the three dimensional mass–metallicity–SFR space, showing that galaxies occupy a clearly defined plane. This plane is shown to be subtly evolving, displaying an increased tilt with time caused by general enrichment, and also the slowing down of star formation with cosmic time. This evolution is most apparent at lookback times greater than 7 Gyr. The trends in metallicity recovered in this work highlight that the evolving metallicity implementation used within the SED fitting code ProSpect produces reasonable metallicity results over the history of a galaxy. This is expected to provide a significant improvement to the accuracy of the SED fitting outputs.

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Section: Introductionmentioning

confidence: 99%

Galaxy and mass assembly (GAMA): the inferred mass–metallicity relation from z = 0 to 3.5 via forensic SED fitting

Bellstedt

Robotham

Driver

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…We are left with a few open questions. As a matter of fact, DDO 68 has an oxygen abundance ∼ 0.8 dex lower than expected for its stellar mass (McQuinn et al 2020, see their Fig. 8): can this metal deficiency be linked to the merger hypothesis?…”

Section: Introductionmentioning

confidence: 91%

“…The field in each panel is 13.8 × 20.7 kpc 2 . Pustilnik et al 2005;Berg et al 2012;McQuinn et al 2020) since it is eXtremely Metal Poor (XMP, Kunth & Östlin 2000;Filho et al 2013;Guseva et al 2015) when compared with dwarf galaxies of similar stellar masses ( 10 8 M , S16) that typically have 12 + log(O/H) ∼ 7.9.…”

Section: Introductionmentioning

confidence: 99%

“…It is generally believed that extremely low metallicities can be the result of dilution of primeval gas recently accreted; or that the metals have been lost due to galactic outflows powered by supernovae explo-sions and stellar winds (Matteucci & Chiosi 1983;Matteucci & Tosi 1985;Marconi et al 1994;Mac Low & Ferrara 1999;Spitoni 2015;Ceverino et al 2016). As for DDO 68, we also need to take into account that the evolution of galaxies within cosmic voids can be very different from that of their counterparts in denser environments (Peebles 2001;Hoeft et al 2006, but see also McQuinn et al 2020). Void galaxies may have evolved more slowly and be metal poorer than galaxies in denser environments because of the absence of merger or gravitational interaction events able to trigger star-formation episodes.…”

Section: Introductionmentioning

confidence: 99%

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Dancing in the void: hydrodynamical N-body simulations of the extremely metal poor galaxy DDO 68

Pascale,

Annibali,

Tosi

et al. 2021

Preprint

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Using hydrodynamical N -body simulations, we show that the observed structure and kinematics of the extremely metal-poor, dwarf irregular galaxy DDO 68 is compatible with a merger event with at least two smaller satellite galaxies. We were able to obtain a self-consistent model that simultaneously reproduces several of its observed features, including: the very asymmetric and disturbed shape of the stellar component, the overall HI distribution and its velocity field, the arc-like stellar structure to the west, the low-surface brightness stellar stream to the north. The model implies the interaction of the main progenitor of DDO 68 with two systems with dynamical masses 7 × 10 8 M and almost 10 8 M -1/20 and 1/150 times the dynamical mass of DDO 68, respectively. We show that the merger between DDO 68 and the most massive of its satellites offers a route to explain the large offset of DDO 68 from the mass-metallicity relation. Assuming that the interacting galaxies have metallicities prior to the merger compatible with those of galaxies with similar stellar masses, we provide quantitative evidence that gas mixing alone does not suffice at diluting the gas of the two components; according to our simulations, the HII regions observed along the Cometary Tail trace the low metallicity of the accreted satellite rather than that of DDO 68's main body. In this case, the mass corresponding to the low metallicity is that of the secondary body and DDO 68 becomes consistent with the mass-metallicity relation.

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“…the Leoncino dwarf; Hirschauer et al 2016); for this galaxy, deeper HST observations were obtained separately in HST-GO-15423. We adopt the distance and galaxy properties reported from this program in McQuinn et al (2020) and discuss these results in more detail below. The CMDs of the galaxies also ubiquitously host upper main sequence and helium burning stars, indicative of recent star formation.…”

Section: Photometry Of the Resolved Starsmentioning

confidence: 99%

Galaxy Properties at the Faint End of the HI Mass Function

McQuinn,

Telidevara,

Fuson

et al. 2021

Preprint

Self Cite

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The Survey of Hi in Extremely Low-mass Dwarfs (SHIELD) includes a volumetrically complete sample of 82 gas-rich dwarfs with M HI 10 7.2 M selected from the ALFALFA survey. We are obtaining extensive follow-up observations of the SHIELD galaxies to study their gas, stellar, and chemical content, and to better understand galaxy evolution at the faint end of the Hi mass function.Here, we investigate the properties of 30 SHIELD galaxies using Hubble Space Telescope imaging of their resolved stars and Westerbork Synthesis Radio Telescope observations of their neutral hydrogen. We measure tip of the red giant branch (TRGB) distances, star formation activity, and gas properties. The TRGB distances are up to 4× greater than estimates from flow models, highlighting the importance of velocity-independent distance indicators in the nearby universe. The SHIELD galaxies are in underdense regions, with 23% located in voids; one galaxy appears paired with a more massive dwarf. We quantify galaxy properties at low masses including stellar and Hi masses, SFRs, sSFRs, SFEs, birthrate parameters, and gas fractions. The lowest mass systems lie below the mass thresholds where stellar mass assembly is predicted to be impacted by reionization. Even so, we find the star formation properties follow the same trends as higher mass gas-rich systems, albeit with a different normalization. The Hi disks are small ( r <0.7 kpc) making it difficult to measure the Hi rotation using standard techniques; we develop a new methodology and report the velocity extent, and its associated spatial extent, with robust uncertainties.

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The Leoncino Dwarf Galaxy: Exploring the Low-metallicity End of the Luminosity–Metallicity and Mass–Metallicity Relations*

Cited by 39 publications

References 98 publications

Galaxy and mass assembly (GAMA): the inferred mass–metallicity relation from z = 0 to 3.5 via forensic SED fitting

Galaxy and mass assembly (GAMA): the inferred mass–metallicity relation from z = 0 to 3.5 via forensic SED fitting

Dancing in the void: hydrodynamical N-body simulations of the extremely metal poor galaxy DDO 68

Galaxy Properties at the Faint End of the HI Mass Function

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