Revision of the New World Heteromeringia (Diptera: Clusiidae: Clusiodinae).

Die 18 neuweltlichen Arten von Heteromeringia Czerny, 1903 werden revidiert inklusive Beschreibung von 10 neuen Arten (H. apholis sp. n. (Mexiko), H. aphotisma sp. n. (Brasilien), H. decora sp. n. (Mexiko), H. lateralis sp. n. (Costa Rica), H. mediana sp. n. (Brasilien), H. nanella sp. n. (Brasilien), H. nervosa sp. n. (Costa Rica), H. quadriseta sp. n. (Ecuador, Peru), H. volcana sp. n. (Costa Rica) und H. zophina sp. n. (Mexiko)). Die nearktische Unterart H. nitida nigripes Melander & Argo, 1924 wird zur Art erhoben. Die H. nitida-Artengruppe und die H. czernyi-Artengruppe werden aufgestellt, und die Verwandtschaftsverhältnisse der letzteren (ausschließlich neotropischen) Gruppe werden diskutiert. Sobarocephala subfasciata Curran, 1939 wird synonymisiert mit H. czernyi Kertesz, 1903. Heteromeringia dimidiata Hennig, 1938 wird in die Gattung Sobarocephala Czerny, 1903 comb. n. gestellt. Heteromeringia tephrinos nomen nov. wird als Ersatzname vorgeschlagen für die afrotropische H. nigrifrons Lamb, 1914, ein jüngeres primäres Homonym von H. nigrifrons Kertesz, 1903. Die Biologie von Heteromeringia wird diskutiert und ein Bestimmungsschlüssel für die neuweltlichen Arten wird vorgestellt. Zum ersten Mal wird aggressives Verhalten innerhalb der Gattung beschrieben: Männchen von H. nitida benutzen ihre zweifarbigen Vorderbeine zur Verteidigung von Paarungsrevieren.StichwörterHeteromeringia, H. czernyi species group, H. nitida species group, Clusiidae, Diptera, New World, revision, new species, stat. n., syn. n., comb. n., nomen n., biology, behaviour.Nomenklatorische Handlungenapholis Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.aphotisma Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.decora Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.flavipes (Williston, 1896) (Heteromeringia), Lectotype described as Heteroneura flavipeslateralis Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.mediana Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.nanella Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.nervosa Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.nigripes Melander & Argo, 1924 (Heteromeringia), stat. n. described as Heteromeringia nitida var. nigripesquadriseta Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.tephrinos Lonsdale & Marshall, 2007 (Heteromeringia), nom. n. pro Heteromeringia nigrifrons Lamb, 1914, nec Kertesz, 1903volcana Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.zophina Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.dimidiata (Hennig, 1938) (Sobarocephala), comb. n. hitherto Heteromeringia dimidiatasubfasciata Curran, 1939 (Sobarocephala), syn. n. of Heteromeringia czernyi Kertesz, 1903The 18 New World species of Heteromeringia Czerny, 1903 are revised, with 10 species described as new: H. apholis sp. n. (Mexico), H. aphotisma sp. n. (Brazil), H. decora sp. n. (Mexico), H. lateralis sp. n. (Costa Rica), H. mediana sp. n. (Brazil), H. nanella sp. n. (Brazil), H. nervosa sp. n. (Costa Rica), H. quadriseta sp. n. (Ecuador, Peru), H. volcana sp. n. (Costa Rica) and H. zophina sp. n. (Mexico). The Nearctic H. nitida nigripes Melander & Argo, 1924 is raised from subspecies to species. The H. nitida species group and the H. czernyi species group are erected, and species relationships are discussed for the latter (entirely neotropical) group. Sobarocephala subfasciata Curran, 1939 is included as a junior synonym of H. czernyi Kertesz, 1903. Heteromeringia dimidiata Hennig, 1938 is moved to Sobarocephala Czerny, 1903 comb. n. Heteromeringia tephrinos nomen n. is provided as a replacement name for the Afrotropical H. nigrifrons Lamb, 1914, which is a junior primary homonym of H. nigrifrons Kertesz, 1903. The biology of Heteromeringia is discussed, and a key is provided for all New World species. Agonistic interactions are described for this genus for the first time, with H. nitida Johnson, 1913 males recorded as using bicoloured forelegs to defend mating territories.KeywordsHeteromeringia, H. czernyi species group, H. nitida species group, Clusiidae, Diptera, New World, revision, new species, stat. n., syn. n., comb. n., nomen n., biology, behaviour.Nomenclatural Actsapholis Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.aphotisma Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.decora Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.flavipes (Williston, 1896) (Heteromeringia), Lectotype described as Heteroneura flavipeslateralis Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.mediana Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.nanella Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.nervosa Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.nigripes Melander & Argo, 1924 (Heteromeringia), stat. n. described as Heteromeringia nitida var. nigripesquadriseta Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.tephrinos Lonsdale & Marshall, 2007 (Heteromeringia), nom. n. pro Heteromeringia nigrifrons Lamb, 1914, nec Kertesz, 1903volcana Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.zophina Lonsdale & Marshall, 2007 (Heteromeringia), spec. n.dimidiata (Hennig, 1938) (Sobarocephala), comb. n. hitherto Heteromeringia dimidiatasubfasciata Curran, 1939 (Sobarocephala), syn. n. of Heteromeringia czernyi Kertesz, 190

Far-Infrared Properties of Spitzer-selected Luminous Starbursts

We present SHARC-2 350 micron data on 20 luminous z ~ 2 starbursts with S(1.2mm) > 2 mJy from the Spitzer-selected samples of Lonsdale et al. and Fiolet et al. All the sources were detected, with S(350um) > 25 mJy for 18 of them. With the data, we determine precise dust temperatures and luminosities for these galaxies using both single-temperature fits and models with power-law mass--temperature distributions. We derive appropriate formulae to use when optical depths are non-negligible. Our models provide an excellent fit to the 6um--2mm measurements of local starbursts. We find characteristic single-component temperatures T1 ~ 35.5+-2.2 K and integrated infrared (IR) luminosities around 10^(12.9+-0.1) Lsun for the SWIRE-selected sources. Molecular gas masses are estimated at 4 x 10^(10) Msun, assuming kappa(850um)=0.15 m^2/kg and a submillimeter-selected galaxy (SMG)-like gas-to-dust mass ratio. The best-fit models imply >~2 kpc emission scales. We also note a tight correlation between rest-frame 1.4 GHz radio and IR luminosities confirming star formation as the predominant power source. The far-IR properties of our sample are indistinguishable from the purely submillimeter-selected populations from current surveys. We therefore conclude that our original selection criteria, based on mid-IR colors and 24 um flux densities, provides an effective means for the study of SMGs at z ~ 1.5--2.5.Comment: 13 pages, 4 figures, edited to match published version in ApJ 717, 29-39 (2010

The Deep SWIRE Field. IV. First properties of the sub-mJy galaxy population: redshift distribution, AGN activity and star formation

We present a study of a 20cm selected sample in the Deep SWIRE VLA Field, reaching a limiting flux density of ~13.5 uJy at the image center. In a 0.6x0.6 square degrees field, we are able to assign an optical/IR counterpart to 97% of the radio sources. Up to 11 passbands from the NUV to 4.5um are then used to sample the spectral energy distribution (SED) of these counterparts in order to investigate the nature of the host galaxies. By means of an SED template library and stellar population synthesis models we estimate photometric redshifts, stellar masses, and stellar population properties, dividing the sample in three sub-classes of quiescent, intermediate and star-forming galaxies. We focus on the radio sample in the redshift range 0.3<z<1.3 where we estimate to have a redshift completeness higher than 90%, and study the properties and redshift evolution of these sub-populations. We find that, as expected, the relative contributions of AGN and star-forming galaxies to the uJy population depend on the flux density limit of the sample. At all flux levels a significant population of "green-valley" galaxies is observed. While the actual nature of these sources is not definitely understood, the results of this work may suggest that a significant fraction of faint radio sources might be composite (and possibly transition) objects, thus a simple "AGN vs star-forming" classification might not be appropriate to fully understand what faint radio populations really are.Comment: 18 pages, 16 figures, accepted for publication in Ap

School physical activity intervention effect on adolescents' performance in mathematics

Purpose: The primary aim of this study was to test the effect of a school-based physical activity intervention on adolescents’ performance in mathematics. A secondary aim was to explore potential mechanisms that might explain the intervention effect. Methods: The Activity and Motivation in Physical EDucation intervention was evaluated using a two-arm cluster randomized controlled trial in 14 secondary schools located in low socioeconomic areas of Western Sydney, Australia. Study participants (n = 1173) were grade 8 students (mean age = 12.94 yr, SD = 0.54). The multicomponent intervention was designed to help teachers maximize students’ opportunities for moderate-to-vigorous physical activity (MVPA) during physical education (PE) and enhance students’ motivation toward PE. Mathematics performance was assessed as part of national testing in grade 7, which was the year before the trial began and then again in grade 9. Potential mediators were: (i) proportion of PE lesson time that students spent in MVPA and leisure time MVPA (%), measured using Actigraph GT3X+ accelerometers, and (ii) students’ self-reported engagement (behavioral, emotional, and cognitive) during mathematics lessons. Mediators were assessed at baseline (grade 8) and follow-up (grade 9, 14–15 months after baseline). Results: The effect of the intervention on mathematics performance was small-to-medium (β = 0.16, P < 0.001). An intervention effect was observed for MVPA% in PE (β = 0.59, P < 0.001), but not for leisure time MVPA or any of the engagement mediators. There were no significant associations between changes in potential mediators and mathematics performance. Conclusions: The Activity and Motivation in Physical EDucation intervention had a significant positive effect on mathematics performance in adolescents. However, findings should be interpreted with caution as the effect was small and not associated with changes in hypothesized mediators

The SWIRE/Chandra Survey: The X-ray Sources

We report a moderate-depth (70 ks), contiguous 0.7 deg^2 Chandra survey in the Lockman Hole Field of the Spitzer/SWIRE Legacy Survey coincident with a completed, ultra-deep VLA survey with deep optical and near-infrared imaging in-hand. The primary motivation is to distinguish starburst galaxies and active galactic nuclei (AGNs), including the significant, highly obscured (log N_H > 23) subset. Chandra has detected 775 X-ray sources to a limiting broadband (0.3-8 keV) flux ~4 × 10^(–16) erg cm^(–2) s^(–1). We present the X-ray catalog, fluxes, hardness ratios, and multi-wavelength fluxes. The log N versus log S agrees with those of previous surveys covering similar flux ranges. The Chandra and Spitzer flux limits are well matched: 771 (99%) of the X-ray sources have infrared (IR) or optical counterparts, and 333 have MIPS 24 μm detections. There are four optical-only X-ray sources and four with no visible optical/IR counterpart. The very deep (~2.7 μJy rms) VLA data yield 251 (>4σ) radio counterparts, 44% of the X-ray sources in the field. We confirm that the tendency for lower X-ray flux sources to be harder is primarily due to absorption. As expected, there is no correlation between observed IR and X-ray fluxes. Optically bright, type 1, and red AGNs lie in distinct regions of the IR versus X-ray flux plots, demonstrating the wide range of spectral energy distributions in this sample and providing the potential for classification/source selection. Many optically bright sources, which lie outside the AGN region in the optical versus X-ray plots (f_r /f_x >10), lie inside the region predicted for red AGNs in IR versus X-ray plots, consistent with the presence of an active nucleus. More than 40% of the X-ray sources in the VLA field are radio-loud using the classical definition, R_L . The majority of these are red and relatively faint in the optical so that the use of R_L to select those AGNs with the strongest radio emission becomes questionable. Using the 24 μm to radio flux ratio (q_(24)) instead results in 13 of the 147 AGNs with sufficient data being classified as radio-loud, in good agreement with the ~10% expected for broad-lined AGNs based on optical surveys. We conclude that q_(24) is a more reliable indicator of radio-loudness. Use of R_L should be confined to the optically selected type 1 AGN

Infrared-Faint Radio Sources: A Cosmological View - AGN Number Counts, the Cosmic X-Ray Background and SMBH Formation

Context. Infrared Faint Radio Sources (IFRS) are extragalactic emitters clearly detected at radio wavelengths but barely detected or undetected at optical and infrared wavelengths, with 5 sigma sensitivities as low as 1 uJy. Aims. Recent SED-modelling and analysis of their radio properties shows that IFRS are consistent with a population of (potentially extremely obscured) high-redshift AGN at 3<z<6. We demonstrate some astrophysical implications of this population and compare them to predictions from models of galaxy evolution and structure formation. Methods. We compiled a list of IFRS from four deep extragalactic surveys and extrapolated the IFRS number density to a survey-independent value of (30.8 +- 15.0) per square degree. We computed the IFRS contribution to the total number of AGN in the Universe to account for the Cosmic X-ray Background. By estimating the black hole mass contained in IFRS, we present conclusions for the SMBH mass density in the early universe and compare it to relevant simulations of structure formation after the Big Bang. Results. The number density of AGN derived from the IFRS density was found to be about 310 deg^-2, which is equivalent to a SMBH mass density of the order of 10^3 M_sun Mpc^-3 in the redshift range 3<z<6. This produces an X-ray flux of 9 10^-16 W m^-2 deg^-2 in the 0.5-2.0 keV band and 3 10^-15 W m^-2 deg^-2 in the 2.0-10 keV band, in agreement with the missing unresolved components of the Cosmic X-ray Background. Concerning the problem of SMBH formation after the Big Bang we find evidence for a scenario involving both halo gas accretion and major mergers.Comment: 8 pages, 4 figures, accepted for publication in A&

A Deep 1.2 mm Map of the Lockman Hole North Field

We present deep 1.2 mm continuum mapping of a 566 arcmin^2 area within the Lockman Hole North field, previously a target of the Spitzer Wide-area Infrared Extragalactic (SWIRE) survey and extremely deep 20 cm mapping with the Very Large Array, which we have obtained using the Max-Planck millimeter bolometer (MAMBO) array on the IRAM 30 m telescope. After filtering, our full map has an RMS sensitivity ranging from 0.45 to 1.5 mJy/beam, with an average of 0.75 mJy/beam. Using the pixel flux distribution in a map made from our best data, we determine the shape, normalization, and approximate flux density cutoff for 1.2 mm number counts well below our nominal sensitivity and confusion limits. After validating our full dataset through comparison with this map, we successfully detect 41 1.2 mm sources with S/N > 4.0 and S(1.2 mm)\simeq 2-5 mJy. We use the most significant of these detections to directly determine the integral number counts down to 1.8 mJy, which are consistent with the results of the pixel flux distribution analysis. 93% of our 41 individual detections have 20 cm counterparts, 49% have Spitzer/MIPS 24 micron counterparts, and one may have a significant Chandra X-ray counterpart. We resolve \simeq 3% of the cosmic infrared background (CIB) at 1.2 mm into significant detections, and directly estimate a 0.05 mJy faint-end cutoff for the counts that is consistent with the full intensity of the 1.2 mm CIB. The median redshift of our 17 detections with spectroscopic or robust photometric redshifts is z(median)=2.3, and rises to z(median)=2.9 when we include redshifts estimated from the radio/far-infrared spectral index. By using a nearest neighbor and angular correlation function analysis, we find evidence that our S/N>4.0 detections are clustered at the 95% confidence level.Comment: 40 pages, 25 figures, accepted for publication in Ap

MAMBO 1.2mm observations of luminous starbursts at z~2 in the SWIRE fields

We report on--off pointed MAMBO observations at 1.2 mm of 61 Spitzer-selected star-forming galaxies from the SWIRE survey. The sources are selected on the basis of bright 24um fluxes (f_24um>0.4mJy) and of stellar dominated near-infrared spectral energy distributions in order to favor z~2 starburst galaxies. The average 1.2mm flux for the whole sample is 1.5+/-0.2 mJy. Our analysis focuses on 29 sources in the Lockman Hole field where the average 1.2mm flux (1.9+/-0.3 mJy) is higher than in other fields (1.1+/-0.2 mJy). The analysis of the sources multi-wavelength spectral energy distributions indicates that they are starburst galaxies with far-infrared luminosities ~10^12-10^13.3 Lsun, and stellar masses of ~0.2-6 x10^11 M_sun. Compared to sub-millimeter selected galaxies (SMGs), the SWIRE-MAMBO sources are among those with the largest 24um/millimeter flux ratios. The origin of such large ratios is investigated by comparing the average mid-infrared spectra and the stacked far-infrared spectral energy distributions of the SWIRE-MAMBO sources and of SMGs. The mid-infrared spectra exhibit strong PAH features, and a warm dust continuum. The warm dust continuum contributes to ~34% of the mid-infrared emission, and is likely associated with an AGN component. This constribution is consistent with what is found in SMGs. The large 24um/1.2mm flux ratios are thus not due to AGN emission, but rather to enhanced PAH emission compared to SMGs. The analysis of the stacked far-infrared fluxes yields warmer dust temperatures than typically observed in SMGs. Our selection favors warm ultra-luminous infrared sources at high-z, a class of objects that is rarely found in SMG samples. Our sample is the largest Spitzer-selected sample detected at millimeter wavelengths currently available.Comment: Accepted for publication in ApJ (51 pages; 16 figures). The quality of some figures has been degraded for arXiv purposes. Full resolution version available at this http://www.iasf-milano.inaf.it/~polletta/mambo_swire/lonsdale08_ApJ_accepted.pd

The star catalogues of Ptolemaios and Ulugh Beg: Machine-readable versions and comparison with the modern Hipparcos Catalogue

In late antiquity and throughout the middle ages, the positions of stars on the celestial sphere were obtained from the star catalogue of Ptolemaios. A catalogue based on new measurements appeared in 1437, with positions by Ulugh Beg, and magnitudes from the 10th-century astronomer al-Sufi. We provide machine-readable versions of these two star catalogues, based on the editions by Toomer (1998) and Knobel (1917), and determine their accuracies by comparison with the modern Hipparcos Catalogue. The magnitudes in the catalogues correlate well with modern visual magnitudes; the indication `faint' by Ptolemaios is found to correspond to his magnitudes 5 and 6. Gaussian fits to the error distributions in longitude / latitude give widths sigma ~ 27 arcmin / 23 arcmin in the range |Delta lambda, Delta beta|<50 arcmin for Ptolemaios and sigma ~ 22 arcmin /18 arcmin in Ulugh Beg. Fits to the range |Delta lambda, Delta beta|<100 arcmin gives 10-15 per cent larger widths, showing that the error distributions are broader than gaussians. The fraction of stars with positions wrong by more than 150 arcmin is about 2 per cent for Ptolemaios and 0.1 per cent in Ulugh Beg; the numbers of unidentified stars are 1 in Ptolemaios and 3 in Ulugh Beg. These numbers testify to the excellent quality of both star catalogues (as edited by Toomer and Knobel).Comment: to be published in Astronomy and Astrophysics; 34 pages with 57 Figures. Note changed address and email address of first autho

A new list of extra-galactic radio jets

A catalogue of extra-galactic jets is very useful both in observational and theoretical studies of active galaxies. With the use of new powerful radio instruments, the detailed structures of very compact or weak radio sources are investigated observationally and many new radio jets are detected. In this paper, we give a list of 661 radio sources with detected radio jets known to us prior to the end of December 2000. All references are collected for the observations of jets in radio, IR, optical, UV and X-ray wave-bands.Comment: 43 pages, 1 figur