The Origin of the Mass‐Metallicity Relation: Insights from 53,000 Star‐forming Galaxies in the Sloan Digital Sky Survey

Tremonti, Christy; Heckman, Timothy M.; Kauffmann, Guinevere; Brinchmann, Jarle; Charlot, S.; White, Simon D. M.; Seibert, Mark; Peng, Eric W.; Schlegel, David J.; Uomoto, Alan; Fukugita, M.; Brinkmann, J.

doi:10.1086/423264

Cited by 3,298 publications

(4,968 citation statements)

References 97 publications

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“…Galaxies are known to follow a mass-metallicity relationship, where the larger the stellar mass the higher the metallicity (e.g., Skillman et al 1989;Tremonti et al 2004;Gallazzi et al 2005). The relationship presents a significant scatter that has been recently found to be associated with the present SFR in the galaxy Lara-López et al 2010;Yates et al 2012;Pérez-Montero et al 2013;Andrews and Martini 2013;Zahid et al 2013).…”

Section: The Stellar Mass-metallicity-sfr Relationshipmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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Section: The Stellar Mass-metallicity-sfr Relationshipmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

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“…those that have the best available spectra). We have restricted our selection to objects having spectral fitting performed by the MPA-JHU group (called the galspec measurements and described in Brinchmann et al 2004;Kauffmann et al 2003b;Tremonti et al 2004).This catalogue has the advantage of including emission line fluxes corrected for Galactic reddening. In addition, through fitting of the observed spectrum with galaxy spectra models, the derived products provide estimates of emission line strengths after subtraction of stellar absorption line components.…”

Section: The Narrow Emission-line Galaxies Samplementioning

confidence: 99%

A new sample of X-ray selected narrow emission-line galaxies

Pons

Watson

2016

A&A

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A sample of X-ray and optically selected narrow emission-line galaxies (769 sources) from the 3XMM catalogue cross-correlated with SDSS (DR9) catalogue has been studied. Narrow-emission line active galactic nuclei (AGN; type-2) have been selected on the basis of their emission line ratios and/or X-ray luminosity. We have looked for X-ray unobscured type-2 AGN. As X-ray spectra were not available for our whole sample, we have checked the reliability of using the X-ray hardness ratio (HR) as a probe of the level of obscuration and we found a very good agreement with full spectral fitting results, with only 2% of the sources with apparently unobscured HR turning out to have an obscured spectrum. Despite the fact that type-2 AGN are supposed to be absorbed based on the Unified Model, about 60% of them show no sign or very low level of X-ray obscuration. After subtraction of contaminants to the sample, that is Narrow-Line Seyfert 1 and Compton-thick AGN, the fraction of unobscured Sy2 drops to 47%. For these sources, we were able to rule out dust reddening and variability for most of them as an explanation of the absence of optical broad emission-lines. The main explanations remaining are the dilution of weak/very broad emission-lines by the host galaxy and the intrinsic absence of the broad-line region (BLR) due to low accretion rates (i.e. True Sy2). However, the number of True Sy2 strongly depends on the method used to verify the intrinsic lack of broad lines. Indeed using the optical continuum luminosity to predict the BLR properties gives a much larger fraction of True Sy2 (about 90% of the unobscured Sy2 sample) than the use of the X-ray 2 keV luminosity (about 20%). Nevertheless the number of AGN we securely detected as True Sy2 is at least three times larger that the previously confirmed number of True Sy2.

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“…Three of the four have relatively low luminosities (−19.3 mag < M r < −18.1 mag), while the host of SN 2008J appears to be consistent with MW luminosity (much like the host of SN 1999E). Turning now to the PTF SNe Ia-CSM, PTF11kx has a latetype spiral host with luminosity comparable to that of the MW and slightly higher-than-solar metallicity (Dilday et al 2012;Tremonti et al 2004). Four of the seven newly discovered SNe Ia-CSM in PTF (PTF10htz, PTF10iuf, PTF11dsb, and PTF12hnr) are also found in what are likely late-type spiral hosts, all of which have luminosities similar to that of the MW (−20.6 mag < M r < −19.2 mag).…”

Section: Host Galaxies Of Sne Ia-csmmentioning

confidence: 99%

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

Silverman¹,

Nugent

Gal‐Yam

et al. 2015

Proc. IAU

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Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the beststudied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogenrich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by Hα emission (with widths of ∼2000 km s −1 ) and exhibit large Hα/Hβ intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He i emission. They also show possible evidence of dust formation through a decrease in the red wing of Hα 75-100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na i D absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be −21.3 mag M R −19 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date.

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The Origin of the Mass‐Metallicity Relation: Insights from 53,000 Star‐forming Galaxies in the Sloan Digital Sky Survey

Cited by 3,298 publications

References 97 publications

Star formation sustained by gas accretion

Star formation sustained by gas accretion

A new sample of X-ray selected narrow emission-line galaxies

Type Ia Supernovae Strongly Interacting with Their Circumstellar Medium

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