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  • 1
    Electronic Resource
    Electronic Resource
    Terpene Compounds as Drugs, XVI. Characterization of the anabolic 19-nortestosterone 17β-trans, trans- and -cis, trans-homofarnesate (1972)
    New York, NY : Wiley-Blackwell
    Helvetica Chimica Acta 55 (1972), S. 1326-1329 
    Details
    ISSN: 0018-019X
    Keywords: Chemistry ; Organic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Notes: 19-Nortestosterone 17β-trans, trans- and -cis, trans-homofarnesate 1 and 2 have been prepared and characterized. Their structure and configuration were identified by mode of formation, elemental analyses, IR. and particularly by NMR. spectra.
    Additional Material: 2 Ill.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1002/hlca.19720550426
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    Paper (German National Licenses)
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  • 2
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    Physical properties of galaxies: towards a consistent comparison between hydrodynamical simulations and SDSS (2016)
    Oxford University Press
    Details
    Publication Date: 2016-08-21
    Description: We study the effects of applying observational techniques to derive the properties of simulated galaxies, with the aim of making an unbiased comparison between observations and simulations. For our study, we used 15 galaxies simulated in a cosmological context using three different feedback and chemical enrichment models, and compared their z = 0 properties with data from the Sloan Digital Sky Survey (SDSS). We show that the physical properties obtained directly from the simulations without post-processing can be very different from those obtained mimicking observational techniques. In order to provide simulators a way to reliably compare their galaxies with SDSS data, for each physical property that we studied – colours, magnitudes, gas and stellar metallicities, mean stellar ages and star formation rates – we give scaling relations that can be easily applied to the values extracted from the simulations; these scalings have in general a high correlation, except for the gas oxygen metallicities. Our simulated galaxies are photometrically similar to galaxies in the blue sequence/green valley, but in general they appear older, passive and with lower metal content compared to most of the spirals in SDSS. As a careful assessment of the agreement/disagreement with observations is the primary test of the baryonic physics implemented in hydrodynamical codes, our study shows that considering the observational biases in the derivation of the galaxies’ properties is of fundamental importance to decide on the failure/success of a galaxy formation model.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 3
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    Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies (2015)
    Oxford University Press
    Details
    Publication Date: 2015-03-22
    Description: Superluminous supernovae (SLSNe) are very bright explosions that were only discovered recently and that show a preference for occurring in faint dwarf galaxies. Understanding why stellar evolution yields different types of stellar explosions in these environments is fundamental in order to both uncover the elusive progenitors of SLSNe and to study star formation in dwarf galaxies. In this paper, we present the first results of our project to study SUperluminous Supernova Host galaxIES, focusing on the sample for which we have obtained spectroscopy. We show that SLSNe-I and SLSNe-R (hydrogen-poor) often (~50 per cent in our sample) occur in a class of galaxies that is known as Extreme Emission Line Galaxies (EELGs). The probability of this happening by chance is negligible and we therefore conclude that the extreme environmental conditions and the SLSN phenomenon are related. In contrast, SLSNe-II (hydrogen-rich) occur in more massive, more metal-rich galaxies with softer radiation fields. Therefore, if SLSNe-II constitute a uniform class, their progenitor systems are likely different from those of H-poor SLSNe. Gamma-ray bursts (GRBs) are, on average, not found in as extreme environments as H-poor SLSNe. We propose that H-poor SLSNe result from the very first stars exploding in a starburst, even earlier than GRBs. This might indicate a bottom-light initial mass function in these systems. SLSNe present a novel method of selecting candidate EELGs independent of their luminosity.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 4
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    SPIDER - X. Environmental effects in central and satellite early-type galaxies through the stellar fossil record (2014)
    Oxford University Press
    Details
    Publication Date: 2014-10-16
    Description: A detailed analysis of how environment affects the star formation history of early-type galaxies (ETGs) is undertaken via high signal-to-noise ratio stacked spectra obtained from a sample of 20 977 ETGs (morphologically selected) from the Sloan Digital Sky Survey-based SPIDER survey. Two major parameters are considered for the study: the central velocity dispersion (), which relates to local drivers of star formation, and the mass of the host halo, which relates to environment-related effects. In addition, we separate the sample between centrals (the most massive galaxy in a halo) and satellites. We derive trends of age, metallicity, and [α/Fe] enhancement, with . We confirm that the major driver of stellar population properties in ETGs is velocity dispersion, with a second-order effect associated with the central/satellite nature of the galaxy. No environmental dependence is detected for satellite ETGs, except at low – where satellites in groups or in the outskirts of clusters tend to be younger than those in the central regions of clusters. In contrast, the trends for centrals show a significant dependence on halo mass. Central ETGs in groups (i.e. with a halo mass 〉10 12.5 M ) have younger ages, lower [α/Fe], and higher internal reddening, than ‘isolated’ systems (i.e. centrals residing in low-mass, 〈10 12.5 M , haloes). Our findings imply that central ETGs in groups formed their stellar component over longer time scales than ‘isolated’ centrals, mainly because of gas-rich interactions with their companion galaxies.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 5
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    The ages of stellar populations in a warm dark matter universe (2014)
    Oxford University Press
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    Publication Date: 2014-04-06
    Description: By means of a semi-analytic model of galaxy formation, we show how the local observed relation between age and galactic stellar mass is affected by assuming a dark matter power spectrum with a small-scale cut-off. We compare results obtained by means of both a cold dark matter (CDM) and a warm dark matter (WDM) power spectrum – suppressed with respect to the CDM at scales below ~1 Mpc. We show that, within a WDM cosmology with a thermal relic particle mass of 0.75 keV, both the mass-weighted and the luminosity-weighted age–mass relations are steeper than those obtained within a CDM universe, in better agreement with the observed relations. Moreover, both the observed differential and cumulative age distributions are better reproduced within a WDM cosmology. In such a scenario, star formation appears globally delayed with respect to the CDM, in particular in low-mass galaxies. The difficulty of obtaining a full agreement between model results and observations is to be ascribed to our present poor understanding of baryonic physics.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 6
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    Measuring the total and baryonic mass profiles of the very massive CASSOWARY 31 strong lens. A fossil system at z ~= 0.7? (2013)
    Oxford University Press
    Details
    Publication Date: 2013-07-14
    Description: We investigate the total and baryonic mass distributions in deflector number 31 (CSWA 31) of the Cambridge And Sloan Survey Of Wide ARcs in the skY (CASSOWARY). We confirm spectroscopically a four-image lensing system at redshift 1.4870 with Very Large Telescope/X-shooter observations. The lensed images are distributed around a bright early-type galaxy at redshift 0.683, surrounded by several smaller galaxies at similar photometric redshifts. We use available optical and X-ray data to constrain the deflector total, stellar and hot gas mass through, respectively, strong lensing, stellar population analysis and plasma modelling. We derive a total mass projected within the Einstein radius R Ein  = 70 kpc of (40 ± 1)  x 10 12  M , and a central logarithmic slope of –1.7 ± 0.2 for the total mass density. Despite a very high stellar mass and velocity dispersion of the central galaxy of (3 ± 1)  x 10 12  M and (450 ± 80) km s –1 , respectively, the cumulative stellar-to-total mass profile of the deflector implies a remarkably low stellar mass fraction of 20 per cent (3–6 per cent) in projection within the central galaxy effective radius R e = 25 kpc ( R  = 100 kpc). We also find that the CSWA 31 deflector has properties suggesting it to be among the most distant and massive fossil systems studied so far. The unusually strong central dark matter dominance and the possible fossil nature of this system render it an interesting target for detailed tests of cosmological models and structure formation scenarios.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 7
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    A new population of recently quenched elliptical galaxies in the SDSS (2014)
    Oxford University Press
    Details
    Publication Date: 2014-06-08
    Description: We use the Sloan Digital Sky Survey to investigate the properties of massive elliptical galaxies in the local Universe ( z  ≤ 0.08) that have unusually blue optical colours. Through careful inspection, we distinguish elliptical from non-elliptical morphologies among a large sample of similarly blue galaxies with high central light concentrations ( c r  ≥ 2.6). These blue ellipticals comprise 3.7 per cent of all c r  ≥ 2.6 galaxies with stellar masses between 10 10 and 10 11 h –2 M . Using published fibre spectrum diagnostics, we identify a unique subset of 172 non-star-forming ellipticals with distinctly blue urz colours and young (〈3 Gyr) light-weighted stellar ages. These recently quenched ellipticals (RQEs) have a number density of 2.7-4.7 x 10 – 5 h 3 Mpc – 3 and sufficient numbers above 2.5 10 10 h –2 M to account for more than half of the expected quiescent growth at late cosmic time assuming that this phase lasts 0.5 Gyr. RQEs have properties that are consistent with a recent merger origin (i.e. they are strong ‘first-generation’ elliptical candidates), yet few involved a starburst strong enough to produce an E+A signature. The preferred environment of RQEs (90 per cent reside at the centres of 〈3 10 12 h –1 M groups) agrees well with the ‘small group scale’ predicted for maximally efficient spiral merging on to their halo centre and rules out satellite-specific quenching processes. The high incidence of Seyfert and LINER activity in RQEs and their plausible descendants may heat the atmospheres of small host haloes sufficiently to maintain quenching.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 8
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    On the two high-metallicity DLAs at z = 2.412 and 2.583 towards Q 0918+1636 (2013)
    Oxford University Press
    Details
    Publication Date: 2013-10-29
    Description: The quasar Q0918+1636 ( z  = 3.07) has two intervening high-metallicity Damped Lyman α Absorbers (DLAs) along the line of sight, at redshifts of z  = 2.412 and 2.583. The z  = 2.583 DLA is located at a large impact parameter of 16.2 kpc, and despite this large impact parameter it has a very high metallicity (consistent with solar), a substantial fraction of H 2 molecules and it is dusty as inferred from the reddened spectrum of the background QSO. The z  = 2.412 DLA has a metallicity of [M/H] = –0.6 (based on Zn ii and Si ii ). In this paper we present new observations of this interesting sightline consisting of deep multiband imaging and further VLT spectroscopy. By fitting stellar population synthesis models to the photometric Spectral Energy Distribution we constrain the physical properties of the z  = 2.583 DLA galaxy, and we infer its morphology by fitting a Sérsic model to its surface brightness profile. We find it to be a relatively massive ( M * 10 10 M ), strongly star-forming (SFR 30 M  yr –1 ), dusty ( E ( B  –  V ) = 0.4) galaxy with a disc-like morphology. We detect strong emission lines from the z  = 2.583 DLA ([O ii ] 3727, [O iii ] 4960, 5007, Hβ and Hα, albeit at low signal-to-noise ratio except for the [O iii ] 5007 line). The metallicity derived from the emission lines is consistent with the absorption metallicity (12 + log (O/H) = 8.8 ± 0.2). We also detect [O iii ] 5007 emission from the galaxy counterpart of the z  = 2.412 DLA at a small impact parameter (〈2 kpc). Overall our findings are consistent with the emerging picture that high-metallicity DLAs are associated with relatively luminous and massive galaxy counterparts, compared to typical DLAs.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 9
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    Comprehensive study of a z = 2.35 DLA Galaxy: mass, metallicity, age, morphology and SFR from HST and VLT (2013)
    Oxford University Press
    Details
    Publication Date: 2013-07-26
    Description: We present a detailed study of the emission from a z  = 2.35 galaxy that causes damped Lyman α absorption in the spectrum of the background quasar (QSO), SDSS J2222–0946. We present the results of extensive analyses of the stellar continuum covering the rest frame optical–UV regime based on broad-band Hubble Space Telescope ( HST) imaging, and of spectroscopy from VLT/X-Shooter of the strong emission lines: Lyα, [O ii ], [O iii ], [N ii ], Hα and Hβ. We compare the metallicity from the absorption lines in the QSO spectrum with the oxygen abundance inferred from the strong-line methods ( R 23 and N2). The two emission-line methods yield consistent results: [O/H] = –0.30 ± 0.13. Based on the absorption lines in the QSO spectrum a metallicity of –0.49 ± 0.05 is inferred at an impact parameter of 6.3 kpc from the centre of the galaxy with a column density of hydrogen of log ( N H I /cm –2 = 20.65 ± 0.05. The star formation rates (SFRs) of the galaxy from the UV continuum and Hα line can be reconciled assuming an amount of reddening of E ( B  – V ) = 0.06 ± 0.01, giving an inferred SFR of 13 ± 1 M yr –1 (Chabrier initial mass function). From the HST imaging, the galaxy associated with the absorption is found to be a compact ( r e  = 1.12 kpc) object with a disc-like, elongated (axis ratio 0.17) structure indicating that the galaxy is seen close to edge-on. Moreover, the absorbing gas is located almost perpendicularly above the disc of the galaxy suggesting that the gas causing the absorption is not corotating with the disc. We investigate the stellar and dynamical masses from spectral energy distribution-fitting and emission-line widths, respectively, and find consistent results of 2  x 10 9 M . We suggest that the galaxy is a young proto -disc with evidence for a galactic outflow of enriched gas. This galaxy hints at how star-forming galaxies may be linked to the elusive population of damped Lyα absorbers.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 10
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    The star formation history of CALIFA galaxies: Radial structures (2014)
    EDP Sciences
    Details
    Publication Date: 2014-02-01
    Print ISSN: 0004-6361
    Electronic ISSN: 1432-0746
    Topics: Physics
    Published by EDP Sciences
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