Citizen-Saints

Lupton, Julia Reinhard

doi:10.7208/chicago/9780226157443.001.0001

Cited by 183 publications

(31 citation statements)

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“…Four of these BCGs have metallicities that fall in the XMD regime. We have calculated the B ‐ and R‐ band magnitudes of the galaxies from their SDSS g and r magnitudes, using the formulae derived by Lupton (2005), which are given on the SDSS web‐site. The parameters of galaxies, in our BCG sample, are given in Table 1.…”

Section: Samplesmentioning

confidence: 99%

When are extremely metal-deficient galaxies extremely metal deficient?

Ekta¹,

Chengalur²

2010

Monthly Notices of the Royal Astronomical Society

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Extremely metal‐deficient (XMD) galaxies, by definition, have oxygen abundances ≤1/10 solar, and form a very small fraction of the local gas‐rich, star‐forming dwarf galaxy population. We examine their positions in the luminosity–metallicity (L–Z) and mass–metallicity (M–Z) planes, with respect to the L–Z and M–Z relations of other gas‐rich, star‐forming dwarf galaxies, viz., blue compact galaxies (BCGs) and dwarf irregular (dI) galaxies. We find that while the metallicities of some low‐luminosity XMD galaxies are consistent with those expected from the L–Z relation, other XMD galaxies are deviant, and more so as the luminosity and/or metal‐deficiency increases. We determine the 95 per cent confidence interval around the L–Z relation for BCGs, and find that its lower boundary is given by 12 + log (O/H) =− 0.177 MB+ 4.87. We suggest that a galaxy should be regarded as XMD, in a statistically significant manner, only if it lies below this boundary in the L–Z plane. Of our sample of XMD galaxies, we find that more than half are XMD by this criterion, and in fact, nine of the galaxies lie below the 99.5 per cent confidence interval about the L–Z relation. We also determine the gas mass fractions and chemical yields of galaxies in all three samples. We find that the effective chemical yield increases with increasing baryonic mass, consistent with what is expected if outflows of metal‐enriched gas are important in determining the effective yield. XMD galaxies have lower effective yield than BCG/dI galaxies of similar baryonic mass. This suggests that some process, peculiar to XMD galaxies, has resulted in their low measured metallicities. Motivated by the fact that interactions are common in XMD galaxies, we suggest that improved (tidally driven) mixing of the interstellar media (ISM) in XMD galaxies leads to a lowering of both, the measured metallicity and the calculated effective yield. In isolated dwarf galaxies, the outer parts of the stellar envelope probably do not participate in the star formation, but are still generally included in the calculation of effective yield. This results in an overestimate of the effective yield. We suggest that XMD galaxies are deviant from the L–Z relation because of a combination of being gas rich (i.e. having processed less gas into stars) and having more uniform mixing of metals in their ISM.

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Section: Samplesmentioning

confidence: 99%

When are extremely metal-deficient galaxies extremely metal deficient?

Ekta¹,

Chengalur²

2010

Monthly Notices of the Royal Astronomical Society

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“…33 Drawing upon Will Kymlicka's distinction between the "thin culture" of liberal pluralism and a "thick" nationalist culture based on ethnic purity, 34 Lupton argues that "Shylock's legal and psychological condition at the end of the play demonstrates the extent to which naturalization in a diverse polity not only can but should remain structurally incomplete, maintaining memories of suspended modes of affiliation that never dissolve completely into a new identity." 35 In Lupton's reading, as well as in my own, Shakespeare is not trying to sell Shylock short but is tacitly configuring and recommending a model of citizenship that resonates very powerfully with the late modern.…”

Section: Portia and The Rabbismentioning

confidence: 94%

Shakespeare in Advance of Hobbes: Pathways to the Modernization of the European Psyche as Charted in The Merchant of Venice

Botwinick¹

2010

Telos

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“…In Figure 4 we plotted the color-color relations for the TRGB of the isochrones for a range of metallicity (−2. Lupton (2005).…”

Section: Data and Data Reductionmentioning

confidence: 99%

Resolving the Discrepancy of Distance to M60, a Giant Elliptical Galaxy in Virgo

Lee

Jang

2017

ApJ

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There is a well-known discrepancy in the distance estimation of M60, a giant elliptical galaxy in Virgo: the planetary nebula luminosity function (PNLF) distance moduli for this galaxy are, on average, 0.4 mag smaller than the values based on the surface brightness fluctuation (SBF) in the literature. We present photometry of the resolved stars in an outer field of M60 based on deep F775W and F850LP images in the Hubble Space Telescope obtained as part of the Pure Parallel Program in the archive. Detected stars are mostly old red giants in the halo of M60. With this photometry, we determine a distance to M60 using the tip of the red giant branch (TRGB). A TRGB is detected at F850LP TRGB = 26.70 ± 0.06 mag, in the luminosity function of the red giants. This value corresponds to F814W 0,TRGB = 27.13 ± 0.06 mag and QT RGB = 27.04 ± 0.07 mag, where QT is a color-corrected F814W magnitude. From this we derive a distance modulus, (m − M ) 0 = 31.05 ± 0.07(ran)± 0.06(sys) (d = 16.23 ± 0.50(ran) ± 0.42(sys) Mpc). This value is 0.3 mag larger than the PNLF distances and 0.1 mag smaller than the SBF distances in the previous studies, indicating that the PNLF distances to M60 in the literature have larger uncertainties than the suggested values.

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Citizen-Saints

Cited by 183 publications

References 0 publications

When are extremely metal-deficient galaxies extremely metal deficient?

When are extremely metal-deficient galaxies extremely metal deficient?

Shakespeare in Advance of Hobbes: Pathways to the Modernization of the European Psyche as Charted in The Merchant of Venice

Resolving the Discrepancy of Distance to M60, a Giant Elliptical Galaxy in Virgo

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