Studies on formaldehyde resins, 25. Kinetic study on the hydroxymethylation of melamine by means of HPLC

Yoshii, Toshio; Konakahara, Takeo; Satô, Kenji

doi:10.1002/macp.1987.021880715

Cited by 56 publications

(67 citation statements)

References 7 publications

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“…However, the chemical enrichment history of a galaxy is thought to depend on factors such as galaxy mass (e.g. Yoshii & Arimoto 1987), and it might be anticipated that the photometric properties of the brightest stars in a massive elliptical galaxy like Maffei 1 might differ from those in a smaller system like M32, due to differences in metallicity. Indeed, the integrated Mg 2 index of M32 is markedly lower than in more massive ellipticals (Burstein et al 1984).…”

Section: The Stellar Content Of Maffei 1 and Other Spheroidsmentioning

confidence: 99%

The Upper Asymptotic Giant Branch of the Elliptical Galaxy Maffei 1 and Comparisons with M32 and NGC 5128

Davidge

2002

The Astronomical Journal

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Deep near-infrared images obtained with adaptive optics (AO) systems on the Gemini North and Canada-France-Hawaii telescopes are used to investigate the bright stellar content and central regions of the nearby elliptical galaxy Maffei 1. Stars evolving on the upper asymptotic giant branch (AGB) are resolved in a field 3 arcmin from the center of the galaxy. The locus of bright giants on the (K, H − K) color-magnitude diagram is consistent with a population of stars like those in Baade's Window reddened by E(H − K) = 0.28 ± 0.05 mag. This corresponds to A V = 4.5 ± 0.8 mag, and is consistent with previous estimates of the line of sight extinction computed from the integrated properties of Maffei 1. The AGB-tip occurs at K = 20.0, which correponds to M K = −8.7; hence, the AGB-tip brightness in Maffei 1 is comparable to that in M32, NGC 5128, and the bulges of M31 and the Milky-Way. The near-infrared luminosity functions (LFs) of bright AGB stars in Maffei 1, M32, and NGC 5128 are also in excellent agreement, both in terms of overall shape and the relative density of infrared-bright stars with respect to the fainter stars that dominate the light at visible and red wavelengths. It is concluded that the brightest AGB stars in Maffei 1, NGC 5128, M32, and the bulge of M31 trace an old, 1 Visiting Astronomer, Canada-France-Hawaii Telescope, which is operated by the National Research Council of Canada, the Centre National de le Recherche Scientifique, and the University of Hawaii.2 Visiting Astronomer, Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Research Council (Canada), the National Science Foundation (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the Australian Reasearch Council (Australia), CNPq (Brazil), and CONICET (Argentina).-2 -metal-rich population, rather than an intermediate age population. It is also demonstrated that Maffei 1 contains a distinct red nucleus, and this is likely the optical signature of low-level nuclear activity and/or a distinct central stellar population. Finally, there is an absence of globular clusters brighter than the peak of the globular cluster LF in the central 700 × 700 parsecs of Maffei 1.

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Section: The Stellar Content Of Maffei 1 and Other Spheroidsmentioning

confidence: 99%

The Upper Asymptotic Giant Branch of the Elliptical Galaxy Maffei 1 and Comparisons with M32 and NGC 5128

Davidge

2002

The Astronomical Journal

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“…Two main different processes have been proposed in the literature. The first mechanism is based on the idea that dEs are formed through internal processes, like supernova feedback, where the interstellar medium (ISM) of the progenitor star-forming galaxy is swept away by the kinetic pressure generated by supernovae (Yoshii & Arimoto 1987), although it seems highly unlikely in dark-matter dominated A&A 526, A114 (2011) systems (Silich & Tenorio-Tagle 2001). The second mechanism rests upon external processes induced by the interaction with the hostile environment in which dEs reside Blanton et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

Toloba

Boselli

Cenarro

et al. 2011

A&A

130

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We present new medium resolution kinematic data for a sample of 21 dwarf early-type galaxies (dEs) mainly in the Virgo cluster, obtained with the WHT and INT telescopes at the Roque de los Muchachos Observatory (La Palma, Spain). These data are used to study the origin of the dwarf elliptical galaxy population inhabiting clusters. We confirm that dEs are not dark matter dominated galaxies, at least not up to the half-light radius. We also find that the observed galaxies in the outer parts of the cluster are mostly rotationally supported systems with disky morphological shapes. Rotationally supported dEs have rotation curves similar to those of star-forming galaxies of similar luminosity and follow the Tully-Fisher relation. This is expected if dE galaxies are the descendants of low-luminosity star-forming systems that have recently entered the cluster environment and lost their gas due to a ram-pressure stripping event, quenching their star formation activity and transforming into quiescent systems, but conserving their angular momentum.

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“…the kinetic energy generated in supernovae sweeps away the gas of the galaxy leaving it without any fuel to create new stars (Yoshii & Arimoto 1987). These processes are not expected to depend on the properties of the surrounding environment.…”

Section: Introductionmentioning

confidence: 99%

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

Toloba

Boselli

Peletier³

et al. 2012

A&A

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We place our sample of 18 Virgo dwarf early-type galaxies (dEs) on the (V − K) e -velocity dispersion, Faber-Jackson, and fundamental plane (FP) scaling relations for massive early-type galaxies (Es). We use a generalized velocity dispersion, which includes rotation, to be able to compare the location of both rotationally and pressure supported dEs with those of early and late-type galaxies. We find that dEs seem to bend the Faber-Jackson relation of Es to lower velocity dispersions, being the link between Es and dwarf spheroidal galaxies (dSphs). Regarding the FP relation, we find that dEs are significantly offset with respect to massive hot stellar systems, and re-casting the FP into the so-called κ-space suggests that this offset is related to dEs having a total mass-to-light ratio higher than Es but still significantly lower than dSph galaxies. Given a stellar mass-to-light ratio based on the measured line indices of dEs, the FP offset allows us to infer that the dark matter fraction within the half light radii of dEs is on average 42% (uncertainties of 17% in the K band and 20% in the V band), fully consistent with an independent estimate in an earlier paper in this series. We also find that dEs in the size-luminosity relation in the near-infrared, like in the optical, are offset from early-type galaxies, but seem to be consistent with late-type galaxies. We thus conclude that the scaling relations show that dEs are different from Es, and that they further strengthen our previous findings that dEs are closer to and likely formed from late-type galaxies.

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Studies on formaldehyde resins, 25. Kinetic study on the hydroxymethylation of melamine by means of HPLC

Cited by 56 publications

References 7 publications

The Upper Asymptotic Giant Branch of the Elliptical Galaxy Maffei 1 and Comparisons with M32 and NGC 5128

The Upper Asymptotic Giant Branch of the Elliptical Galaxy Maffei 1 and Comparisons with M32 and NGC 5128

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

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