Sepsis Causes Loss of Cd3 T Cells, B Cells, and Lymphoid Follicles.

Tinsley, Kevin W.; Swanson, Paul E.; Coopersmith, Craig; Wagner, Teagan; Schmieg, Robert E.; Chang, Kathy; Osborne, Dale F.; Freeman, Bailey E.; Cobb, J. Perren; Buchman, Timothy G.; Karl, Ingolf; Hotchkiss, Richard

doi:10.1097/00024382-200106001-00054

Cited by 2 publications

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“…Tinsley 1972) that continuous mass-loss from old stars could lead to the formation of younger generations of stars in early-type galaxies. The far ultraviolet excess observed in the central region of M31 (Code & Hoag 1969), first tentatively attributed to E-mail: herpich@astro.ufsc.br hot, highly evolved stars (Hills 1971), was later suggested to arise from hot young main-sequence stars (Tinsley 1971). Various ionization sources for the emission-line gas observed in elliptical galaxies were considered, such as decay of turbulence or ultraviolet radiation from hot stars (Osterbrock 1960).…”

Section: Introductionmentioning

confidence: 99%

Why do many early-type galaxies lack emission lines? I. Fossil clues

Herpich

Stasińska

Mateus

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Early-type retired galaxies (RGs, i.e. galaxies which no longer form stars) can be divided into two classes: those with no emission lines, here dubbed lineless RGs, and those with emission lines, dubbed liny RGs. Both types of galaxies contain hot lowmass evolved stars (HOLMES) which emit ionizing photons. The difference must thus lie in the presence or absence of a reservoir of ionizable gas. From a volume-limited sample of 38 038 elliptical galaxies, we explore differences in physical properties between liny and lineless using data from the SDSS, WISE and GALEX catalogues. To avoid biases in the comparison, we pair-match liny and lineless in stellar-mass, redshift and half-light Petrosian radius. We detect marginal differences in their optical stellar ages and NUV luminosities, indicating that liny RGs have an excess of intermediateage (0.1-5 Gyr) stellar populations. Liny RGs show higher dust attenuation and W 3 luminosities than their lineless counterparts. We also find that the amount of warm gas needed to explain the observed Hα luminosity in liny RGs is 10 5 -10 8 M , and that their [N ii]/[O ii] emission-line ratios are typical of those of the most massive star-forming galaxies. Taken together, these results rules out the following sources for the warm gas in liny RGs: mass-loss from intermediate-mass stars, mergers with metal-poor galaxies and intergalactic streams. They imply instead an inflow of enriched gas previously expelled from the galaxy or a merger with a metal-rich galaxy. The ionization source and the origin of the gas producing the emission lines are thus disconnected.

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Section: Introductionmentioning

confidence: 99%

Why do many early-type galaxies lack emission lines? I. Fossil clues

Herpich

Stasińska

Mateus

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…This is of particular importance because the energy output at different wavelengths is dominated by stars of different masses. While galaxy luminosities measured in the ultraviolet are sensitive to the energy output of hot, short-living O and B type stars and, therefore, to ongoing star formation (Tinsley 1971;Madau et al 1996Madau et al , 1998, the optical and NIR luminosities provide constraints on more evolved stellar populations (Hunter et al 1982). This can be used, in principle, to derive the evolution of such basic galaxy properties as the stellar mass function (see e.g.…”

Section: Introductionmentioning

confidence: 99%

The evolution of the luminosity functions in the FORS deep field from low to high redshift

Gabasch

Hopp

Feulner

et al. 2006

A&A

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We present the redshift evolution of the restframe galaxy luminosity function (LF) in the red r , i , and z bands, as derived from the FORS Deep Field (FDF), thus extending our earlier results to longer wavelengths. Using the deep and homogeneous I-band selected dataset of the FDF, we were able to follow the red LFs over the redshift range 0.5 < z < 3.5. The results are based on photometric redshifts for 5558 galaxies derived from the photometry in 9 filters and achieving an accuracy of ∆z/(z spec + 1) ≤ 0.03 with only ∼1% outliers. A comparison with results from the literature shows the reliability of the derived LFs. Because of the depth of the FDF, we can give relatively tight constraints on the faint-end slope α of the LF; the faint-end of the red LFs does not show a large redshift evolution and is compatible within 1σ to 2σ with a constant slope over the redshift range 0.5 < ∼ z < ∼ 2.0. Moreover, the slopes in r , i , and z are very similar to a best-fitting value of α = −1.33 ± 0.03 for the combined bands. There is a clear trend of α to steepen with increasing wavelength: α UV&u = −1.07 ± 0.04 → α g &B = −1.25 ± 0.03 → α r &i &z = −1.33 ± 0.03. We subdivided our galaxy sample into four SED types and determined the contribution of a typical SED type to the overall LF. We show that the wavelength dependence of the LF slope can be explained by the relative contribution of different SED-type LFs to the overall LF, as different SED types dominate the LF in the blue and red bands. Furthermore we also derived and analyzed the luminosity density evolution of the different SED types up to z ∼ 2. We investigated the evolution of M * and φ * by means of the redshift parametrization M * (z) = M * 0 + a ln (1 + z) and φ * (z) = φ * 0 (1 + z) b . Based on the FDF data, we found only a mild brightening of M * (a r ∼ −0.8, and a i ,z ∼ −0.4) and a decreasing φ * (b r ,i ,z ∼ −0.6) with increasing redshift. Therefore, from z ∼ 0.5 to z ∼ 3 the characteristic luminosity increases by ∼0.8, ∼0.4, and ∼0.4 mag in the r , i , and z bands, respectively. Simultaneously the characteristic density decreases by about 40% in all analyzed wavebands. A comparison of the LFs with semianalytical galaxy formation models by Kauffmann et al. (1999) shows a similar result to the blue bands: the semi-analytical models predict LFs that describe the data at low redshift very well, but show growing disagreement with increasing redshifts.Article published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx.

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Sepsis Causes Loss of Cd3 T Cells, B Cells, and Lymphoid Follicles.

Cited by 2 publications

References 0 publications

Why do many early-type galaxies lack emission lines? I. Fossil clues

Why do many early-type galaxies lack emission lines? I. Fossil clues

The evolution of the luminosity functions in the FORS deep field from low to high redshift

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