An extended Herschel drop-out source in the center of AS1063: a normal dusty galaxy at z=6.1 or SZ substructures?

In the course of our 870 μm APEX/LABOCA follow-up of the Herschel Lensing Survey we have detected a source in AS1063 (RXC J2248.7-4431) that has no counterparts in any of the Herschel PACS/SPIRE bands, it is a Herschel “drop-out” with S_870/S_500 ≥ 0.5. The 870 μm emission is extended and centered on the brightest cluster galaxy, suggesting either a multiply imaged background source or substructure in the Sunyaev-Zel’dovich increment due to inhomogeneities in the hot cluster gas of this merging cluster. We discuss both interpretations with emphasis on the putative lensed source. Based on the observed properties and on our lens model we find that this source may be the first submillimeter galaxy (SMG) with a moderate far-infrared (FIR) luminosity (L_FIR < 10^12 L_⊙) detected so far at z > 4. In deep HST observations we identified a multiply imaged z ~ 6 source and measured its spectroscopic redshift to be z = 6.107 with VLT/FORS. This source may be associated with the putative SMG, but it is most likely offset spatially by 10−30 kpc and they may be interacting galaxies. With a FIR luminosity in the range [5−15] × 10^11 L_⊙ corresponding to a star formation rate in the range [80−260] M_⊙ yr^-1, this SMG would be more representative of the z > 4 dusty galaxies than the extreme starbursts detected so far. With a total magnification of ~25 it would open a unique window to the normal dusty galaxies at the end of the epoch of reionization.

On the Analytic Solutions of the Functional Equations w 1 f(a 1 z) + w 2 f(a 2 z) + ... + w n f(a n z) = 0

In this paper, it is showed that, given an integer number n ≥ 2, each zero of an exponential polynomial of the form w1az1+w2az2+⋯+wnazn, with non-null complex numbers w 1,w 2,…,w n and a 1,a 2,…,a n , produces analytic solutions of the functional equation w 1 f(a 1 z) + w 2 f(a 2 z) + ... + w n f(a n z) = 0 on certain domains of C, which represents an extension of some existing results in the literature on this functional equation for the case of positive coefficients a j and w j.

Majmūʻah: 1. al-Qāḍī maʻa al-manhīyāt, 2. al-Ḥāshiyah li-Mawlānā Muḥammad Yūsuf, 3. al-Ḥāshiyah li-Mawlānā Ḥāfiẓ Darrāz, 4. al-Sullam maʻa al-Tanbīhāt

Lithographed.

Sexage et phylogénie, à partir des gènes CHD (-Z et -W) et COX-1, des oiseaux de proie du Québec et de perroquets d’attrait vétérinaire

Connaître le sexe d’un oiseau est important pour divers domaines notamment pour les vétérinaires, les écologistes ainsi que pour les éleveurs d’oiseaux qui veulent former des couples qui serviront à la reproduction. Plusieurs espèces d’oiseaux, juvéniles et adultes, n’ont pas de dimorphisme sexuel. L’utilisation de l’ADN est une façon rapide de déterminer le sexe à partir d’un échantillon de sang, de muscle, de plumes ou de fèces. Par contre, la méthode devrait être validée pour chaque espèce et idéalement, standardisée. Le premier objectif de cette étude est de développer une méthode de sexage par séquençage des oiseaux à partir des séquences du gène CHD, en utilisant les oiseaux de proie et les perroquets vus en clinique au Québec. Un deuxième objectif est de faire l’identification de l’espèce à sexer, à partir du gène mitochondrial COX-1 et aussi à partir des séquences CHD-Z et CHD-W, utilisés pour le sexage. Un troisième objectif est d’évaluer les séquences sorties (CHD-Z, CHD-W et COX-1) en vue d’une étude phylogénique. Une extraction d’ADN a été effectuée chez 27 espèces de perroquets, 34 espèces d’oiseaux de proie, une corneille (Corvus brachyrhynchos) et un poulet (Gallus gallus). Une amplification par PCR a été exécutée pour les exons partiels 23 et 24 du gène CHD. Le séquençage de cet amplicon permettait de savoir s’il s’agissait d’un mâle (séquence simple CHD-Z) ou d’une femelle (séquences CHD-Z et CHD-W qui se chevauchent). Afin d’avoir des séquences CHD-W distinctes, un sous-clonage a été fait chez les femelles de chaque espèce. De cette manière, les séquences partielles du gène CHD, Z et W, ont été trouvées pour les espèces échantillonnées. Une étude phylogénique a été effectuée avec les séquences de COX-1, CHD-Z et CHD-W grâce au site « Clustal-Omega ». La méthode de sexage des oiseaux par séquençage du gène CHD est standard et efficace. Le gène COX-1 permet une meilleure identification des espèces parentes et le gène CHD-Z est le plus utile pour étudier la phylogénie profonde.

Pamĕti nejvyššího kancléře království Českého Viléma hraběte Slavaty, z Chlumu a z Košmberka ... šenka království Českého, císařuʺv Ferdinanda II. a III. ... (nar. 1. prosince 1572, zemř. 19. ledna 1652) Od \U+25a1\. 1608 do 1619 /

Includes indexes.

The 2dF-SDSS LRG and QSO (2SLAQ) survey: the z < 2.1 quasar luminosity function from 5645 quasars to g=21.85

We have used the Two-Degree Field (2dF) instrument on the Anglo-Australian Telescope (AAT) to obtain redshifts of a sample of z < 3 and 18.0 < g < 21.85 quasars selected from Sloan Digital Sky Survey (SDSS) imaging. These data are part of a larger joint programme between the SDSS and 2dF communities to obtain spectra of faint quasars and luminous red galaxies, namely the 2dF-SDSS LRG and QSO (2SLAQ) Survey. We describe the quasar selection algorithm and present the resulting number counts and luminosity function of 5645 quasars in 105.7 deg(2). The bright-end number counts and luminosity functions agree well with determinations from the 2dF QSO Redshift Survey (2QZ) data to g similar to 20.2. However, at the faint end, the 2SLAQ number counts and luminosity functions are steeper (i.e. require more faint quasars) than the final 2QZ results from Croom et al., but are consistent with the preliminary 2QZ results from Boyle et al. Using the functional form adopted for the 2QZ analysis ( a double power law with pure luminosity evolution characterized by a second-order polynomial in redshift), we find a faint-end slope of beta =-1.78 +/- 0.03 if we allow all of the parameters to vary, and beta =-1.45 +/- 0.03 if we allow only the faint-end slope and normalization to vary (holding all other parameters equal to the final 2QZ values). Over the magnitude range covered by the 2SLAQ survey, our maximum-likelihood fit to the data yields 32 per cent more quasars than the final 2QZ parametrization, but is not inconsistent with other g > 21 deep surveys for quasars. The 2SLAQ data exhibit no well-defined 'break' in the number counts or luminosity function, but do clearly flatten with increasing magnitude. Finally, we find that the shape of the quasar luminosity function derived from 2SLAQ is in good agreement with that derived from Type I quasars found in hard X-ray surveys.

The Las Campanas/Anglo-Australian Telescope Rich Cluster Survey - III. Spectroscopic studies of X-ray bright galaxy clusters at z similar to 0.1

We present the analysis of the spectroscopic and photometric catalogues of 11 X-ray luminous clusters at 0.07 < z < 0.16 from the Las Campanas/Anglo-Australian Telescope Rich Cluster Survey. Our spectroscopic data set consists of over 1600 galaxy cluster members, of which two-thirds are outside r(200). These spectra allow us to assign cluster membership using a detailed mass model and expand on our previous work on the cluster colour-magnitude relation ( CMR) where membership was inferred statistically. We confirm that the modal colours of galaxies on the CMR become progressively bluer with increasing radius d( B - R)/dr(p) = - 0.011 +/- 0.003 and with decreasing local galaxy density d( B - R)/dlog ( Sigma)= - 0.062 +/- 0.009. Interpreted as an age effect, we hypothesize that these trends in galaxy colour should be reflected in mean H delta equivalent width. We confirm that passive galaxies in the cluster increase in Hd line strength as dH delta/dr(p) = 0.35 +/- 0.06. Therefore, those galaxies in the cluster outskirts may have younger luminosity-weighted stellar populations; up to 3 Gyr younger than those in the cluster centre assuming d( B - R)/dt = 0.03 mag per Gyr. A variation of star formation rate, as measured by [ O II]lambda 3727 angstrom, with increasing local density of the environment is discernible and is shown to be in broad agreement with previous studies from the 2dF Galaxy Redshift Survey and the Sloan Digital Sky Survey. We divide our spectra into a variety of types based upon the MORPHs classification scheme. We find that clusters at z similar to 0.1 are less active than their higher-redshift analogues: about 60 per cent of the cluster galaxy population is non-star forming, with a further 20 per cent in the post-starburst class and 20 per cent in the currently active class, demonstrating that evolution is visible within the past 2 - 3 Gyr. We also investigate unusual populations of blue and very red non-star forming galaxies and we suggest that the former are likely to be the progenitors of galaxies which will lie on the CMR, while the colours of the latter possibly reflect dust reddening. We show that the cluster galaxies at large radii consist of both backsplash ones and those that are infalling to the cluster for the first time. We make a comparison to the field population at z similar to 0.1 and examine the broad differences between the two populations. Individually, the clusters show significant variation in their galaxy populations which we suggest reflects their recent infall histories.

Organic reactions in ionic liquids; Ionic liquid-accelerated three-component reaction: a rapid one-pot synthesis of 3-alkyl-5-[(Z)-arylmethylidene]-1,3-thiazolidine-2,4-diones

A rapid one-pot synthesis of 3-alkyl-5-[(Z)-arylme­thylidene]-1,3-thiazolidine-2,4-dionesis described that occurs in recyclable ionic liquid [bmim]PF6 (1-butyl-3-methylimidazolium hexafluorophosphate).Significant rate enhancement and good selectivity have been observed.

The host galaxies and black holes of typical z~0.5-1.4 AGNs

We study the stellar and star formation properties of the host galaxies of 58 X-ray-selected AGNs in the GOODS portion of the Chandra Deep Field South (CDF-S) region at z ~ 0.5-1.4. The AGNs are selected such that their rest-frame UV to near-infrared spectral energy distributions (SEDs) are dominated by stellar emission; i.e., they show a prominent 1.6 μm bump, thus minimizing the AGN emission "contamination." This AGN population comprises approximately 50% of the X-ray-selected AGNs at these redshifts. We find that AGNs reside in the most massive galaxies at the redshifts probed here. Their characteristic stellar masses (M_* ~ 7.8 × 10^10 and M_* ~ 1.2 × 10^11 M_☉ at median redshifts of 0.67 and 1.07, respectively) appear to be representative of the X-ray-selected AGN population at these redshifts and are intermediate between those of local type 2 AGNs and high-redshift (z ~ 2) AGNs. The inferred black hole masses (M_BH ~ 2 × 10^8 M_☉) of typical AGNs are similar to those of optically identified quasars at similar redshifts. Since the AGNs in our sample are much less luminous (L_2–10 keV < 10^44 erg s^−1) than quasars, typical AGNs have low Eddington ratios (η ~ 0.01-0.001). This suggests that, at least at intermediate redshifts, the cosmic AGN "downsizing" is due to both a decrease in the characteristic stellar mass of typical host galaxies and less efficient accretion. Finally, there is no strong evidence in AGN host galaxies for either highly suppressed star formation (expected if AGNs played a role in quenching star formation) or elevated star formation when compared to mass-selected (i.e., IRAC-selected) galaxies of similar stellar masses and redshifts.

Mid-infrared spectroscopy of lensed galaxies at 1 < z < 3: The nature of sources near the MIPS confusion limit

We present Spitzer IRS mid-infrared spectra for 15 gravitationally lensed, 24 μm-selected galaxies, and combine the results with four additional very faint galaxies with IRS spectra in the literature. The median intrinsic 24 μm flux density of the sample is 130 μJy, enabling a systematic survey of the spectral properties of the very faint 24 μm sources that dominate the number counts of Spitzer cosmological surveys. Six of the 19 galaxy spectra (32%) show the strong mid-IR continuua expected of AGNs; X-ray detections confirm the presence of AGNs in three of these cases, and reveal AGNs in two other galaxies. These results suggest that nuclear accretion may contribute more flux to faint 24 μm-selected samples than previously assumed. Almost all the spectra show some aromatic (PAH) emission features; the measured aromatic flux ratios do not show evolution from z = 0. In particular, the high signal-to-noise mid-IR spectrum of SMM J163554.2+661225 agrees remarkably well with low-redshift, lower luminosity templates. We compare the rest-frame 8 μm and total infrared luminosities of star-forming galaxies, and find that the behavior of this ratio with total IR luminosity has evolved modestly from z = 2 to z = 0. Since the high aromatic-to-continuum flux ratios in these galaxies rule out a dominant contribution by AGNs, this finding implies systematic evolution in the structure and/or metallicity of infrared sources with redshift. It also has implications for the estimates of star-forming rates inferred from 24 μm measurements, in the sense that at z ~ 2, a given observed frame 24 μm luminosity corresponds to a lower bolometric luminosity than would be inferred from low-redshift templates of similar luminosity at the corresponding rest wavelength.

Exercise and lymphoedema : Is it good or bad?

Being physically active during and following treatment for breast cancer has been associated with a range of benefits including improved fitness and function, body composition and immune function and reductions in stress, depression and anxiety, as well as the number and severity of treatment-related side-effects such as nausea, fatigue and pain, all of which contribute to improvements in quality of life. There is also emerging evidence linking active lifestyles with improved survival. Therefore, there is little doubt that participating in regular exercise following breast cancer is ‘good’. Unfortunately, research investigating the role of exercise for women considered at high-risk of lymphoedema or who have developed lymphedema following breast cancer is lacking. For fear of initiating or exacerbating lymphoedema, these women have traditionally been cautioned rather than encouraged to be regularly active. However, recent preliminary findings suggest that being inactive may increase risk of developing lymphedema, and that for those with lymphoedema, participation in an exercise program does not exacerbate the condition. This presentation will address what we know about the role of exercise following a breast cancer diagnosis and will provide some practical recommendations about becoming and staying regularly active following breast cancer, for those with and without lymphoedema.

Show me a bad kid and I’ll show you a lousy parent : making parents responsible for youth crime in Australian and Canadian Contexts

This article surveys literature bearing on the issue of parental liability and responsibility for the crimes of young offenders, with a particular focus on comparing different approaches to dealing with the issue in Australia and Canada. This comparative analysis of Australian and Canadian legislative and policy approaches is situated within a broader discussion of arguments about the “punitive turn” in youth justice, responsibilisation, and cross-jurisdictional criminal justice policy transfer and convergence. Our findings suggest that there are significant differences in the manner and extent to which Australia and Canada have invoked parental responsibility laws and policies as part of the solution to dealing with youth crime. We conclude by speculating on some of the reasons for these differences and establishing an agenda for additional needed cross-jurisdictional research. In particular, we argue that it would be fruitful to undertake a cross-jurisdictional study that examines the development and effects of parental responsibility laws across a larger number of different Western countries as well as across individual states and provinces within these national jurisdictions.

The structure of the copper(II) complex with 4,5-dichlorophthalic acid: The 1:1 complex 'adduct' salt trans-tetraaqua(2-carboxy-4,5-dichlorobenzoato)(4,5-dichlorobenzene-1,2-dicarboxylic acid)copper(II) 2-carboxy-4,5-dichlorobenzoate

The unusual (1:1) complex ‘adduct’ salt of copper(II) with 4,5-dichlorophthalic acid (H2DCPA), having formula [Cu(H2O)4(C8H3Cl2O4) (C8H4Cl2O4)] . (C8H3Cl2O4) has been synthesized and characterized using single-crystal X-ray diffraction. Crystals are monoclinic, space group P21/c, with Z = 4 in a cell with dimensions a = 20.1376(7), b =12.8408(4) c = 12.1910(4) Å, β = 105.509(4)o. The complex is based on discrete tetragonally distorted octahedral [CuO6] coordination centres with the four water ligands occupying the square planar sites [Cu-O, 1.962(4)-1.987(4) Å] and the monodentate carboxyl-O donors of two DCPA ligand species in the axial sites. The first of these bonds [Cu-O, 2.341(4) Å] is with an oxygen of a HDCPA monoanion, the second with an oxygen of a H2DCPA acid species [Cu-O, 2.418(4) Å]. The un-coordinated ‘adduct’ molecule is a HDCPA counter anion which is strongly hydrogen-bonded to the coordinated H2DCPA ligand [O… O, 2.503(6) Å] while a number of peripheral intra- and intermolecular hydrogen-bonding interactions give a two-dimensional network structure.