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Home All issues Volume 556 (August 2013) A&A, 556 (2013) A119 Full HTML
Volume 556, August 2013
Interstellar and circumstellar matter
2. The sample
3. Observations
4. Data analysis
6. Investigation of ...
A&A 556, A119 (2013)
Submillimeter observations of IRAS and WISE debris disk candidates⋆
J. Bulger1, T. Hufford2, A. Schneider2, J. Patience1,3, I. Song2, R. J. De Rosa3, A. Rajan3, C. D. Dowell4, D. McCarthy5 and C. Kulesa5
1 School of Physics, University of Exeter, Exeter, EX4 6LZ, UK
e-mail: joanna@astro.ex.ac.uk
2 Department of Physics and Astronomy, The University of Georgia, Athens, GA 30602-2451, USA
3 School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85281, USA
4 Department of Physics and Astronomy, Caltech, MC 249-17, Pasadena, CA 91125, USA
5 The Department of Astronomy and Steward Observatory, The University of Arizona, Tucson, AZ 85721, USA
A set of six debris disk candidates identified with IRAS or WISE excesses were observed at either 350 μm or 450 μm with the Caltech Submillimeter Observatory. Five of the targets – HIP 51658, HIP 68160, HIP 73512, HIP 76375, and HIP 112460 – have among the largest measured excess emission from cold dust from IRAS in the 25–100 μm bands. Single temperature blackbody fits to the excess dust emission of these sources predict 350–450 μm fluxes above 240 mJy. The final target – HIP 73165 – exhibits weak excess emission above the stellar photosphere from WISE measurements at 22 μm, indicative of a population of warm circumstellar dust. None of the six targets were detected, with 3σ upper limits ranging from 51–239 mJy. These limits are significantly below the expected fluxes from SED fitting. Two potential causes of the null detections were explored – companion stars and contamination. To investigate the possible influence of companion stars, imaging data were analyzed from new adaptive optics data from the ARIES instrument on the 6.5 m MMT and archival HST, Gemini NIRI, and POSS/2MASS data. The images are sensitive to all stellar companions beyond a radius of 1–94 AU, with the inner limit depending on the distance and brightness of each target. One target is identified as a binary system, but with a separation too large to impact the disk. While the gravitational effects of a companion do not appear to provide an explanation for the submm upper limits, the majority of the IRAS excess targets show evidence for contaminating sources, based on investigation of higher resolution WISE and archival Spitzer and Herschel images. Finally, the exploratory submm measurements of the WISE excess source suggest that the hot dust present around these targets is not matched by a comparable population of colder, outer dust. More extensive and more sensitive Herschel observations of WISE excess sources will build upon this initial example to further define the characteristics of warm debris disks sources.
Key words: submillimeter: planetary systems / circumstellar matter / stars: imaging / techniques: high angular resolution
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
© ESO, 2013
Debris disks were first identified with the Infrared Astronomical Satellite (IRAS), from the observation that the far-IR flux of Vega (Aumann et al. 1984) was significantly brighter than expected from the stellar photosphere. Excess emission above the level of a stellar photosphere at wavelengths from the mid-IR to the millimeter provides evidence of reprocessed starlight emitted by a circumstellar debris disk of dust (see reviews by Zuckerman 2001; Wyatt 2008). The disk origin of these excesses has been confirmed with spatially resolved imaging (e.g. Smith & Terrile 1984; Holland et al. 1998). Given the timescale for the dust to spiral into the star or be ejected from the system, these dust disks must be sustained by an ongoing process such as the collisional grinding of planetesimals into smaller particles (Backman & Paresce 1993) or an event such as a catastrophic collision of planets (Cameron 1997).
Observed sample.
While IRAS provided an all-sky survey for debris disks with a typical sensitivity of (Ldust/L⋆) ~ 10-5, subsequent pointed observations from the Spitzer Space Telescope (Werner et al. 2004), achieved an order of magnitude greater sensitivity. The combined results of the all-sky and pointed observations have identified over 200 debris disks among field stars (e.g. Mannings & Barlow 1998; Moór et al. 2006; Rhee et al. 2007; Habing et al. 1999; Silverstone 2000; Rieke et al. 2005; Su et al. 2006; Bryden et al. 2006; Beichman et al. 2006; Hillenbrand et al. 2008; Carpenter et al. 2009). Assuming a single temperature blackbody model for the excess emission in the spectral energy distribution (SED), it is possible to classify debris disks as warm (equivalent to that of our Asteroid belt), with Tdust ≈ 100–250 K, that lie at distances ≲10 AU, and cold debris disks (equivalent to that of our Kuiper belt), with Tdust ≲ 50 K, typical distances of several hundred AU.
With the more recent Herschel and Wide-field Infrared Survey Explorer (WISE) missions, it is possible to conduct pointed searches for cold debris disks down to the Kuiper belt level (Ldust/L⋆) ~ 10-7 to 10-6 (Stern 1996) and all-sky surveys for warm debris disks at a sensitivity level that was previously only obtained with Spitzer pointed observations. In addition to the sensitivity offered by both Herschel and WISE, the significant improvement of spatial resolution is important to identify possible sources of contamination. Examples of debris disks identified through IRAS excesses (e.g. Moór et al. 2006; Rhee et al. 2007) that are actually due to confusion from background source contamination have been revealed by higher resolution ground-based observations carried out in the IR and submm (e.g. Song et al. 2002; Jayawardhana et al. 2002; Lisse et al. 2002; Sheret et al. 2004).
Mid-IR to far-IR observations have been critical in identifying the current population of debris disks, however measurements at longer wavelengths in the submm/mm wavelength range provide the best means to estimate one of the most important properties of a disk, the dust mass. For disks that are spatially resolved in the submm, it is also possible to determine additional disk characteristics such as size and inclination which are degenerate with other disk parameters in an SED fit. For disks that have imaged asymmetries, these structures can encode the effects of gravitational interactions (e.g. Liou & Zook 1999; Kuchner & Holman 2003; Wyatt 2006; Quillen & Faber 2006). The submm/mm wavelength range is ideal for studying the interaction of the disk and planets, i.e. in the case of the multiple planet, debris disk system around HR8799 (e.g. Patience et al. 2011; Hughes et al. 2011), since the large grains are expected to remain in resonances with the planets, while the smaller grains evolve into axisymmetric structures due to scattering or radiation pressure (Wyatt 2006).
In this paper, we present the results of a submm and IR imaging study of several IRAS excess stars and one WISE excess star. This sample includes previously known systems with cold dust (Moór et al. 2006; Rhee et al. 2007) and newly identified debris disk candidates with evidence of either cold or warm dust. The properties of the sample are summarized in Sect. 2. The single-dish submm observations, infrared imaging and archival searches are described in Sect. 3. In Sect. 4, the data reduction and analysis of our submm and IR observations is presented. The results and implications of the IR image analysis is given in Sect. 5. In Sect. 6, we draw comparisons of our investigation to previous submm studies of debris disks. Finally, the conclusions of our study are given Sect. 7.
SEDs of the cold debris disk source candidates for which the submm flux limits are substantially below the extension of the single temperature blackbody fit to the IRAS excesses – HIP 51658, HIP 68160, HIP 76375 and HIP 112460. The NextGen atmospheric models corresponding to the best-fit stellar photosphere and the blackbody fit are plotted. The optical-near IR photometric points (black points) have been compiled from Tycho2 and 2MASS. The mid-IR photometric points have been drawn from WISE (dark blue points). For HIP 51568, with Herschel PACS photometry, the orange points with downward arrows correspond to the source 3σ upper limits. The orange points represent the cumulative flux density of three nearby contaminating objects. For HIP 76375 and HIP 112460, with Spitzer MIPS photometry, the green points represent the source flux density and green points with downward arrows represent the source 3σ upper limits. The flux density of the contaminating object measured in the MIPS 70 μm image for HIP 76375 is represented by the light-blue point. The CSO submm flux upper limit at 350 or 450 μm are represented by the pink points with downward arrows.
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Submillimeter observations.
The target sample for this investigation of cold and warm excess debris disks is drawn from two main sources – the IRAS Faint Source Catalog (FSC v.2) (Moshir et al. 1992) and results from the WISE All-Sky Data Release (Cutri & et al. 2012). We selected a sample of cold excess disk candidates from the literature (Lestrade et al. 2006; Moór et al. 2006; Rhee et al. 2007) that satisfy three criteria: (1) a large IRAS excesses at 60 μm or 100 μm; (2) a distance within 100 pc; and (3) a declination above –30°. SEDs were constructed, and a single temperature blackbody model was fit to the IRAS excesses. Targets with an expected 350 μm flux greater than 100 mJy were considered for this study, and the SEDs of the targets are shown in Figs. 1 and 2. Due to weather considerations, we focused our observations on sources with the greatest predicted 350 μm flux and and with nearby distances (<40 pc), in order to obtain meaningful limits and have the capacity to resolve the disks of the nearest systems. A total of 5 cold debris disks candidates were observed in this study, and are listed in Table 1, along with a summary of the modelled dust properties from the literature. The second type of target with evidence for warmer dust was drawn from the WISE (3.4 μm, 4.6 μm, 12 μm, and 22 μm) All-Sky Data Release. The identification of a WISE W3 (12 μm) and/or W4 (22 μm) band excess was based on a careful cross-correlation of the WISE and Hipparcos catalogues (Perryman & ESA 1997; van Leeuwen 2007) with a distance cut of 100 pc and an estimate of the photospheric flux from theoretical atmosphere models (Hauschildt et al. 1999). Due to the limited clear weather windows during the observing runs, it was only possible to observe one warm excess source – HIP 73615. HIP 73615 has an excess only in the WISE W4 band, and the excess above the photosphere is 34 times the uncertainty in the photometry. The properties of the target are listed in Table 1, and the SED for this warm debris disk candidate is plotted in Fig. 3.
3.1. Submillimeter observations
Observations of the six sources were made with the SHARCII bolometer array (Dowell et al. 2003) on the 10.4 m Caltech Submillimeter Observatory (CSO) on Mauna Kea. SHARCII contains a 12 × 32 array of pop-up bolometers with a >90% filling factor over the field and provides background-limited 350 μm and 450 μm maps. For the closest systems, we obtained 350 μm maps to potentially resolve the disks. For the remaining targets we measured 450 μm maps to measure longer wavelength fluxes distinct from the Herschel bands. Table 2 which wavelengths were observed for each source and the exposure times. The field-of-view of the SHARCII maps was ~2′ × 0 6, and the beam sizes at 350 μm and 450 μm are ~8 5 and ~10 0, respectively. The beam shape was stabilized by the active primary surface correction (Leong et al. 2006), which corrects for dish surface imperfections and changes in the gravity vector as a function of elevation.
The data were acquired during two observing runs: February 14–22 2012 and June 6–14 2012. There were no significant changes to the instrument over the course of the project. The conditions during the observations ranged from excellent τ225 GHz = 0.03 to marginal τ225GHz = 0.07. The observing sequence consisted of a series of target scans bracketed by scans of planets and nearby secondary calibrators, serving as both absolute flux calibration and pointing calibration measurements. Table 2 lists the calibrators observed for each science target. Pointing calibration measurements were taken at least once per hour during the observing period and focus corrections were monitored throughout the night. Typical individual target scan times were 620 s, while 120 s was sufficient for the calibrators. A total of 1 to 11 scans were taken on the science targets.
High resolution imaging observations.
SED of the cold debris disk candidate – HIP 73512 for which the submm flux limit lies above the extension of the single temperature blackbody fit to the IRAS excesses. The NextGen atmospheric model corresponding to the best-fit stellar photosphere and the blackbody fit are plotted. Deeper submm observations for are required to further assess this source as a cold debris disk candidate.
SED of our WISE excess source – HIP 73165. The NextGen atmospheric model corresponding to the best-fit stellar photosphere is plotted. Excess is seen in the W4 band above the photosphere, and is 34 times the uncertainty in the photometry. The CSO 450 μm 3σ upper limit (pink point and downwards arrow) shows the level to which lack of submm excess emission is seen.
Field plate image of HIP 76375, the only source in our sample with a known companion. The orientation is indicated with the arrows, along with a scale bar for this 8′ × 4′ image. The companion – HIP 76382, identified from CPM (Shaya & Olling 2011) is labeled on the image and lies 148° from the primary, with a separation of 121 8. The IRAS FSC positional uncertainty for HIP 76375 is displayed on the image (red ellipse).
3.2. Imaging observations
High angular resolution observations were used to search for the presence of a stellar binary companion to each member of the sample, since a companion can impact the stability of debris disk material. Dedicated observations were obtained for four targets with the Arizona Infrared Imager and Echelle Spectrograph (ARIES; McCarthy et al. 1998) at the 6.5 m AO-equipped MMT on December 23, 2012. The observing strategy was the same for each target, with a series of short unsaturated exposures taken first to calibrate the photometry of the observing sequence, followed by deep exposures in which the core of the PSF of the target was saturated, increasing the sensitivity to faint stellar companions. For both sets of exposures, images were obtained at a series of offset positions to measure the sky background and mitigate the effects of bad pixels. Additionally, the CFHT and HST archives were searched for previous high angular resolution observations of each sample member. Collectively, the new and archival observations include all the targets. Details of the high angular resolution observations of the sample are given in Table 3.
To increase the range of separations at which a stellar binary companion can be detected to a limit of 10 000 AU, digitized photographic plates were obtained from the SuperCosmos Sky Survey Science Archive (Hambly et al. 2001) for each target within the sample. For the targets within 30 pc, several of the 15′ × 15′ digitized plates were combined to ensure the angular coverage was sufficient to detect co-moving companions with separations up to the 10 000 AU outer boundary considered for this study. The large time baseline between the first and last photographic observation, combined with the high proper motion of the sample members, allowed for an identification of wide common proper motion (CPM) companions. An example of one of the wide-field images is shown in Fig. 4.
The WISE All-Sky Survey Atlas images and IRAS Sky Survey Atlas (ISSA) for all the sources of our sample. The images are displayed per source (repented by the row heading) in order of survey, and the wavelength of observation from left to right (indicated by the column heading). Orientation for all images are north, up and east, left. The WISE images are 400′′ × 300′′ in size. The spatial resolution of the ISSA images at each wavelength are smoothed to the IRAS 100 μm beam size and are 900′′ × 900′′ in size. The black circles represent the IRAS 100 μm beam centered over the source positions. The sources and the wavelengths for which IRAS FSC upper limits are reported are indicted in the images. The four cold debris disks candidates with submm limits well below the SED fit are HIP 51658, HIP 61680 and HIP 76357 and HIP 112460, and are investigated for the possibility of contaminating sources within the IRAS beam. For HIP 51658, HIP 61680 and HIP 76357 nearby objects are visible in the higher resolution WISE images (see also Fig. 6). Additionally, for HIP 76357, the secondary companion (HIP 76382) is seen dominant in all WISE images and is noticeably seen in the 12 μm and 25 μm ISSA images. No contaminating sources are visible in either the WISE or ISSA images for HIP 112460.
3.3. Archival mid-IR/far-IR images
For each target, images from the all-sky surveys of IRAS and WISE were obtained for this program. Figure 5 shows the region centered on each target for each of the four bands of WISE (left) and four bands of IRAS (right). Overplotted on each image is the approximate size of the 100 μm IRAS beam; the beam is estimated as circular using the average of the elliptical major and minor axis as the radius. We searched the Spitzer Heritage Archive and the Herschel Science Archive for higher resolution, pointed far-IR observations for each target, and three of the targets have additional higher resolution data. Level 2 MIPS data at 24 μm and 70 μm were retrieved for HIP 76375 and HIP 112460, and level 2.5 PACS data at 100 and 160 μm was retrieved for HIP 51658. The pointed observations with Spitzer and Herschel are shown in Fig. 6.
4.1. Submm maps and fluxes
The analysis of the CSO 350 μm and 450 μm data included four main steps: application of a pointing model1, reduction of the raw data with the CRUSH pipeline (Kovács 2006, 2008), measurement of aperture photometry, and calibration of fluxes. As an initial step, the pointing drifts of the telescope were estimated for each observation with a pointing model that accounts for both static effects, measured with many pointing sources at different positions throughout the run, and for time variable effects, measured with pointing sources observed before and after the science target. These offsets and the contemporaneous measurement of the atmospheric opacity are then incorporated into the data processing, implemented with the CRUSH (version 2.11-2) software (Kovács 2006, 2008). The output of CRUSH includes an intensity map and signal-to-noise ratio map. The image processing algorithm is optimized depending on source brightness. We utilized the data reduction settings appropriate to the flux levels for the planets, pointing sources and science targets. Circular apertures with a radius of 9 5 at 350 μm and 10 6 at 450 μm were used for the target photometry; the aperture sizes are based on the measured FWHM of the point source calibrator at each wavelength.
Absolute fluxes of the planets are based on the distance from the Earth and the Sun, calculated at the time of observation and determined using the planetary brightness temperatures measured by Griffin & Orton (1993). The planets Mars, Neptune and Uranus were used for primary flux calibration and have absolute calibration uncertainties of ~5–10% (Griffin & Orton 1993). For nights without a planet observation, the calibration is tied to the secondary calibrators Arp 220, CRL 618 and OH 231.8. For observations at 350 μm, we use a flux density of 23.3 ± 4.2 Jy for CRL 618 (derived by Dowell and listed on the SHARCII website2). The uncertainty is based on the long term variability of evolved stars (Sandell 2003; Jenness et al. 2002). At 450 μm, we use a flux density of 6.3 ± 0.8 mJy for Arp220 (Dunne & Eales 2001), 12.1 ± 2.2 mJy for CLR 618 and 12.7 ± 2.2 mJy for OH 231.8 (Jenness et al. 2002). The uncertainty of the flux calibration is combined with the uncertainty of the source signal which is measured from the CRUSH source maps. The total uncertainty on the submm fluxes of the science targets ranges from ~15–30%.
None of the six targets were detected in the CSO 350 μm or 450 μm maps. We have therefore pursued two types of analysis in order to investigate the causes for these null detections, presented in Sect. 5. With infrared imaging, we investigate the possible disruptive effects caused by companion stars and with an analysis of available mid-IR to far-IR maps, we explore the possibility of source contamination in the IRAS catalogue resulting in a misidentification of the target as a debris disk system.
Higher resolution IR images for the sources – HIP 51568, HIP 61680 and HIP 76375, in which nearby contaminating objects are seen in the WISE and when available Spitzer MIPS and Herschel PACS images. The orientation for all images are north, up and east, left and the images are 300′′ in size along each axis. The black circles represent the IRAS 100 μm beam centered over the source positions. For HIP 51658 a nearby object (~55″ to the NE) is seen to become increasingly brighter at increasing wavelengths, as shown in the WISE 22 μm (W4) and Herschel PACS 100 μm images. For HIP 68160, a nearby object (~35″ to the west) is seen in the W4 image. For HIP 76375 and the binary companion – HIP 76382 (121′′ to the SE) are both visible in the WISE 3.4 μm (W1), W4 and Spitzer MIPS 24 μm images. Neither component of the system are seen in the Spitzer MIPS 70 μm image. The galaxy IC 4563 (~80″ to the east), is visible in the W4 and MIPS images, and lies within the IRAS beam area.
4.2. High resolution and wide-field, near-IR/optical companion search images
For the ground-based AO images from the MMT and CFHT, we performed standard image processing steps to account for sky background and detector dark current, nonlinearity, bad pixels, and quantum efficiency variations. The individual science images were aligned, and median combined. For the HST archive data, the images were already reduced and flux calibrated, so no additional processing was required. Each final target image was searched for stellar companions, and detection limits were calculated as a function of separation. For each target, the minimum separation at which a stellar companion at the bottom of the main sequence (0.08 M⊙) could be detected was determined. The variance of the pixel values within the science images was measured as a function of separation, scaled by the flux and apparent magnitude of the central target, and compared to the expected apparent magnitude of a 0.08 M⊙ stellar companion obtained from theoretical models (Baraffe et al. 1998).
Three of the sample members have also been searched for binary companions with speckle interferometry (HIP 51658, HIP 76375, and HIP 112460; Miura et al. 1995; Hartkopf & Mason 2009; Balega et al. 2007), and none of which were found to have a binary companion. While these techniques would be sensitive to a high mass ratio binary companion at close separations, their sensitivity does not extend to the bottom of the main sequence. Future observations with increased sensitivity are required in order to rule out the presence of any stellar companion interior to the detection limits given in Table 5.
To search for companions beyond the field-of-view of the high angular resolution instruments, the digitized photographic plates for each target were blinked to reveal the presence of any wide co-moving companions. To ensure wide CPM companions were not missed during the visual inspection, the PPMXL (Roeser et al. 2010) and the UCAC4 (Zacharias et al. 2012) catalogues were also searched for stars with proper motions consistent with the object being physically bound to the primary.
4.3. IRAS data
We visually inspected each image in order to assess the quality and association of IRAS Faint Source Catalogue fluxes that have been extracted for the targets. The synthesized beam sizes of the Faint Source Survey images are approximately 1′ × 4′ at 12 μm and 25 μm, 2′ × 4′ and 4′ × 5′ at 60 μm and 100 μm, respectively. The positional uncertainties of IRAS detections for our sample is ~3′′ in the in-scan direction and ~18′′ in the cross-scan direction. In addition, we have reassessed the quality of the FSC extracted flux densities for our targets, with the use of the online Scan Processing and Integration (SCANPI) tool3. SCANPI combines the signal for all (in-scan) survey scans that correspond to the target position and provides fluxes of faint sources, estimates of true local upper limits and deviation of the signal peak to that of the source position. Despite the stringent processing of the survey scans and catalog criteria that have been implemented for source extraction and identification, the large angular resolution of the IRAS beams is one of the primary factors of possible source contamination.
4.4. Higher resolution mid-far IR WISE, Spitzer and Herschel images
WISE provides a factor of 10 higher resolution images in the mid-IR than IRAS. The WISE beam sizes are 6 1, 6 4, 6 5 and 12′′ at 3.4 μm (W1), 4.6 μm (W2), 12 μm (W3) and 22 μm (W4). To utilize this significant improvement of resolution, we performed visual cross inspection of the four WISE bands, to identify any contaminating objects that are contained within the IRAS beam sizes. Additionally, we investigated the available Spitzer MIPS and Herschel PACS (Poglitsch et al. 2010) processed images from the archive for the targets HIP 76375, HIP 112460, and HIP 51658. HIP 68160 was not observed by either Spitzer or Herschel. The Spitzer FWHM beam size with MIPS at 24 μm is 6′′, a factor two greater than the WISE W4 band, and pointed observations further increase the sensitivity beyond that achieved with the WISE survey. The far-IR MIPS channels at 70 μm and 160 μm, with corresponding beam sizes of 20″ and 40″, and the Herschel PACS channels at 70 μm, 100 μm and 160 μm, with FWHM beam sizes of 5 6, 6 8 and 11 4 respectively, provide the far-IR wavelength coverage with significantly greater resolution than that of IRAS, enabling the identification of contaminating objects such as background galaxies that become increasingly brighter across the mid-far IR regime.
Submillimeter detection limits.
Companion search results.
None of the six debris disk targets were detected in the CSO SHARCII maps. The 3σ upper limits range from 31 mJy for HIP 51658 to 239 mJy for HIP 73512 at 450 μm, and all the limits are reported in Table 4. For four of the five cold debris disks targets, the submm flux limits are substantially below the extension of the blackbody fit to the IRAS excesses, as shown in Fig. 1. The CSO limit for the cold debris disk candidate HIP 73512 is above the blackbody fit, as shown in Fig. 2, and the CSO data do not constrain the disk in this case. The WISE excess source HIP 73165 also shows a lack of submm emission at a level reported in Table 4 and plotted on the SED in Fig. 3.
5.1. CSO flux limits
The flux limits were converted into dust mass limits following previous submm studies (e.g. Zuckerman & Becklin 1993) using the expression Md = (FνD2)/Bν(T)κν, where the blackbody function Bν(T) is equal to 2kT/λ2 in the Rayleigh-Jeans limit. The dust opacity at the frequency of observation κν assumes a functional form κν = κ0(ν/ν0)β at submm wavelengths. We use a normalization value κ0 = 0.17 m2 kg-1 at 850 μm and scale with β = 1 (Zuckerman & Becklin 1993; Pollack et al. 1994). Existing submm studies find that β = 1 is a representative value of debris disks (Dent et al. 2000) and the normalization value for dust opacity is adopted for direct comparison with previous studies (e.g. Sylvester et al. 2001; Wyatt et al. 2003; Liu et al. 2004; Sheret et al. 2004; Najita & Williams 2005; Williams & Andrews 2006). Assuming an average dust temperature of 30 K for the submm-emitting dust, the submm flux limits correspond to dust mass limits of 0.001 to 0.261 M⊕, as reported in Table 4. These dust mass limits are comparable to the detections of other nearby debris disks based on either submm fluxes or fits to IRAS fluxes over a large wavelength range (e.g. compilation in Rhee et al. 2007).
The submm upper limits are plotted along with previous measurements at shorter wavelengths to construct the SEDs of the IRAS cold excess debris disks with limits below the blackbody fit in Fig. 1 and with a limit above the blackbody fit in Fig. 2. The WISE warm excess debris disk SED is plotted in Fig. 3. For the cold excess sources, the fits to the 60–100 μm emission, assuming a single temperature blackbody, are also shown for comparison with the measured CSO limits. For the targets HIP 51658, HIP 68160, HIP 76375 and HIP 112460, the submm limits are all well below the expected flux level at these wavelengths, making these limits more restrictive than previous submm measurements of some debris disks candidates Williams & Andrews (2006). For the WISE source, there is not a large enough wavelength coverage for the excess emission to perform a fit, and the exploratory measurement at the longer wavelength is shown in comparison to the newly reported mid-IR excess in the WISE W4 band. With only an excess in the longest wavelength WISE band, it is not possible to fit a blackbody to estimate an expected flux level for the CSO measurement, but the non-detection is consistent with a spatially confined distribution of hot dust for this source. Larger scale studies with more sensitive limits from Herschel will provide more definitive constraints on the origin of WISE excesses for sources such as HIP 73165.
5.2. Companion systems
Since a companion star will gravitationally truncate the outer portion of a disk and reduce the amount of submm-emitting dust, all targets were searched for stellar companions. A visual inspection of the high-resolution data did not reveal any companion candidates. Separately, a visual inspection of each of the blinked image pairs combined with a search of the astrometric catalogues, identified one co-moving object – the known wide CPM companion to HIP 76375 (Shaya & Olling 2011). The HIP 76375 system is shown in Fig. 4. The binary separation is 121 8, which corresponds to a projected physical separation of ~2700 AU – too large to impact the disk size unless the orbit is very eccentric and periastron passage occurs at a much smaller separation. Table 5 lists the details of the HIP 76375 binary system and the closest separation at which the data become sensitive to companions at the bottom of the main sequence for each of the targets. The minimum separation ranges from only 1 AU for the M-star HIP 112460 at ~5 pc to 94 AU for the more massive and more distant A-star HIP 51658 at ~30 pc. In addition to the the companion search we performed, five targets were included in the interferometric (van Belle et al. 2008; van Belle 2010) and speckle (Hartkopf & McAlister 1984; Miura et al. 1995; Hartkopf & Mason 2009; Balega et al. 2007) searches, and no companions were discovered for these targets, although the detection limits were not deep enough to include all possible stellar companions.
5.3. IRAS source contamination
For the four cold debris disk candidates with submm limits well below the SED fit (shown in Fig. 1), we investigated the possibility of contaminating sources within the IRAS beam. All targets have WISE images in four bands with higher resolution than IRAS, and three of the four targets have Spitzer data in at least one bandpass. Three of the four objects – HIP 51658, HIP 61680, and HIP 76375 – show contaminating sources in the higher resolution mid-IR/far-IR images shown in Fig. 6. Only one – HIP 112460 – shows a single object in the higher resolution WISE and Spitzer maps shown in Fig. 7. The results of the contamination analysis for these sources is discussed in the following subsections.
5.3.1. HIP 51658
From the sequence of WISE images for HIP 51658 in Figs. 5 and 6, a nearby object ~55′′ to the NE of HIP 51658 is seen and becomes increasingly brighter with wavelength. Also shown in Fig. 6 is the Herschel PACS 100 μm map centered on the target which reveals the offset source, but not the target. In both the WISE and Herschel maps there are additional fainter sources within the IRAS beam (not visible with the scaling of Fig. 6). Three distinct sources are detected in the Herschel 100 μm map. From our SCANPI analysis of this source, we find that signals are significant in all IRAS bands (>5σ) and the the deviation from source position to the signal peak is <0.5′.
To determine the flux of the contaminating objects, we have measured the flux densities of the nearby three objects that fall within the IRAS beam centered over the source position, and find that the cumulative flux density at 100 μm is consistent with the IRAS FSC 100 μm flux. Furthermore, the 160 μm cumulative flux density fits well to the single temperature blackbody, modelled excess fit. The PACS fluxes, along with our 450 μm upper limit that lies significantly below the fit, are shown in Fig. 1. This analysis indicates that the associated IRAS 60 μm and 100 μm fluxes of this source are contaminated and that HIP 51658 is not a bona fide debris disk system. To determine more accurate flux upper limits for HIP 51658, we have extracted level 2.5 processed PACS 100 μm and 160 μm images from the Herschel archive and measured 3σ flux upper limits of 22 mJy at 100 μm and 34 mJy at 160 μm, following the point source photometry guidelines recommended by the Herschel team4.
As shown in Fig. 6, a nearby object ~35′′ to the west of HIP 68160 is visible in the W4 22 μm image, and lies within the IRAS beam. The IRAS 25 μm flux for this source is reported as an upper limit in the FSC. As there are no higher resolution far-IR observations available from Spitzer or Herschel for this source, we are unable to quantify the level of flux contamination within the IRAS 60 μm and 100 μm bands, unlike the case of HIP 51658. The presence of the additional source in the WISE W4 image does, however, suggest that the IRAS fluxes are heavily influenced by this red object. Based on this second source in the field, HIP 68160 is also a probable case of a misclassified debris disk system.
Higher resolution Spitzer MIPS images for HIP 112460. The orientation of both images are north, up and east, left and the images are 300′′ in size along each axis. The black circles represent the IRAS 100 μm beam centered over the source position. The source is clearly detected in the 24 μm image, with no visible nearby contaminating objects. The 3σ upper limit of the source measured in the 70 μm image lies well below the modelled, single blackbody excess fit. Whilst stripping artifacts are seen in the 70 μm image no nearby contaminating objects are visible.
This target is the only known binary in our sample. Both the target and binary companion (separation of 121 8) are visible in all four WISE images (see Fig. 5) and the MIPS 24 μm image (see Fig. 6). From our SCANPI analysis we note that there is a large positional offset (1.9′) from the source to signal peak in the IRAS 12 μm band, with a SNR of 8. Figure 5 shows the IRAS scans at 12 μm, 60 μm and 100 μm. In the 12 μm scan, the position of the binary companion falls on the peak emission pixel, indicating that the IRAS 12 μm flux reported for this source contaminated is from emission of the secondary.
To investigate the longer wavelength measurements, we have extracted the archival MIPS images at 24 μm and 70 μm for this source, shown in Fig. 6. In all the WISE images and in the MIPS 24 μm image, both the target and companion are visible. The galaxy, IC 456345 (~80′′ to the E) is seen to become increasingly brighter with longer wavelengths, as seen in Figs. 5 and 6. In the MIPS 70 μm image, neither the source or companion are visible, yet the galaxy is clearly seen and lies within the IRAS 100 μm beam, centered over the source position. The SNR of the signal, returned with SCANPI at 60 μm is marginal at 2.9σ and the positional offset from the source to signal peak is 0.33′. Whilst this offset is below the FSC criteria to flag the source as an upper limit, it is significantly greater than that of other 60 μm source detections (as determined through comparison of our sources and those of a similar study i.e. Williams & Andrews 2006 – as is discussed in Sect. 6).
From the MIPS images we have measured the source flux at 24 μm, the 3σ upper limit at 70 μm, and the flux of the galaxy (light blue point); included on the SED shown in Fig. 1. We find that the source 24 μm flux lies on the modelled photosphere of this object and that the 70 μm upper limit lies significantly below the single blackbody, model excess fit. Furthermore, we find that the 70 μm flux of the galaxy matches well to the excess fit. In visual inspection of the IRAS scans it can be seen that at the position of the galaxy, the corresponding pixel becomes increasingly brighter at longer wavelengths. From this analysis, we conclude that both the IRAS 60 μm and 100 μm flux is contaminated due to the emission from the galaxy.
5.3.4. HIP 112460
Although the HIP 112460 M-star cold debris disk candidate has the largest discrepancy between the predicted submm flux from the SED and the measured CSO limit (a factor of ~100), no additional source was identified within the IRAS beam. From inspection of the higher resolution WISE and MIPS images, no contaminating object is detected in the surrounding field of this source, as shown in Fig. 7. Due to the low latitude of the source (b = −13°), it is possible that the associated 100 μm IRAS flux is contaminated from Galactic cirrus emission. Another possibility for this nearby source is a dilution of the flux from a disk due to a spatially resolved disk. To assess the impact of a spatially resolved disk, we searched for the largest reported spatially resolved disks around M-stars (AU Mic – MacGregor et al. 2013, and GJ 581 – Lestrade et al. 2012), scaled the disk size based on the distance to HIP 112460, and determined the number of beams across which the flux would be distributed in a uniform disk. Even for the larger of the two resolved M-star disks, the resulting size at the distance of HIP 112460 would spread the flux across ~9 beams, diluting the flux by a factor too small to account for the large discrepancy.
Another possible explanation for the submm non-detection is a variable source. Some support for this hypothesis comes from the conflicting flux measurements at different epochs, since the fluxes obtained from later observations with WISE at 12 μm and 22 μm and Spitzer MIPS at 24 μm fall on the photosphere of the star, compared to the excesses obtained from the earlier IRAS at 12 and 25 μm scans, and seen at high significance at 12 μm and 100 μm in Fig. 5. From the Spitzer MIPS images of this source, we measured the 24 μm flux and the 70 μm upper limit. As shown in Fig. 1, the Spitzer 24 μm flux lies on the modelled stellar photosphere for this source and both the 3σ upper limits at 70 μm and our 350 μm observation, lie well below the modelled, single blackbody excess fit (unlike the IRAS values). A large scale IRAS variability investigation of blazars (Impey & Neugebauer 1988) did find sources with variability up to an order of magnitude at 100 μm, however such a large amplitude change was very rare. Another example of a large degree of variability intrinsic to a debris disk at somewhat shorter wavelengths in the mid-IR was reported for the TYC 8241 2652 1 debris disk (Melis et al. 2012) which exhibited a remarkable change of a factor of ~30 over a timescale of less than two years. More observations are required to provide further understanding into the nature of this unusual, possibly variable, system.
6. Investigation of other debris disks with upper limits
The high rate of source contamination of the IRAS FSC fluxes found amongst our cold debris disk sample prompted us to conduct the same contamination analysis for a previous submm study, at 850 μm of eight debris disks (Williams & Andrews 2006), to further assess the likelihood of additional examples of misidentified debris disks. In the Williams & Andrews (2006) study, the sources were selected through IRAS FSC excesses, similar to our program. Upper-limits were obtained for two of the eight sources – HD 56099 and HD 78702. From inspection of the higher resolution WISE and Spitzer MIPS images of these two sources, we find that a nearby object lies within the IRAS beam size for HD 56099. No nearby contaminating objects are visible in either the WISE or Spitzer images for HD 78702. For HD 56099, the nearby object is visible in the WISE W3 and W4 images and in the MIPS 24 μm, 70 μm and 160 μm images, and becomes increasingly brighter with wavelength. Moór et al. (2006) identify this source to be a misclassified debris disk system, due to the nearby object contamination as identified, and Moór et al. (2011) have further analysed the Spitzer observations for this target and find a low significance level of excess above that of the stellar photosphere. One out of eight sources, in the study carried out by Williams & Andrews (2006), was misidentified of possessing a cold debris disk. Comparatively, for the cold debris disk sample within this paper, three out of the five sources show evidence of nearby object contamination of the associated IRAS FSC fluxes.
We have presented new submm observations at either 350 μm or 450 μm, searching for dust emission around a sample of cold and warm nearby (<40 pc) debris disk candidates that have been identified from IRAS or WISE excesses.
Upper-limits were obtained for all six targets, and four of the limits are well below the expected submm flux, based on a single temperature blackbody model fit to previous shorter wavelength photometry. Of the four cold excess sources with very discrepant submm limits compared to the SED fit, we found that three targets have clearly identified contaminating objects in the IRAS beam, and, therefore, are likely misidentified debris disk candidates. Quantitive measurements of the contaminating objects were obtained for two targets – HIP 51658 and HIP 76375 – from higher resolution, pointed Herschel PACS and Spitzer MIPS observations at wavelengths comparable to the IRAS excess fluxes. From visual inspection of the WISE all-sky survey images, we find that HIP 61680 is also like to suffer from IRAS contamination, in which we identify a nearby, background object that becomes increasingly brighter over the WISE bands as the likely true source of the IRAS FSC measurement.
The rate of IRAS contamination has likely lead to a greater number of sources in being identified as possessing cold debris disks than the actual number. Considering the high level of source contamination in this study and comparable results from an analysis of other debris disks candidates with submm non-detections (Williams & Andrews 2006), lower detection rates than anticipated for large scale debris disks surveys that are currently being pursued with Herschel and SCUBA2 may be found.
It is important to highlight the need for careful examination of source contamination for observations in the far-IR and submm wavelengths, where the probability of detecting a nearby background source can be as high as 36% (Booth et al. 2013; Berta et al. 2011). In this study we find 4–5 examples of contamination either from identified objects or possible background variability, giving a contamination rate of 31–38% similar to the probability reported in Booth et al. (2013).
Finally, we note that it is only now that it is possible to assess systematically the IRAS associations of debris disk candidates by using the complementary mid-IR to far-IR wavelength coverage and higher resolution and sensitivity provided by WISE, Spitzer and Herschel.
http://www.submm.caltech.edu/~sharc/analysis/pmodel
http://www.submm.caltech.edu/~sharc/
http://irsa.ipac.caltech.edu/applications/Scanpi/
Technical Note PICC-ME-TN-037 in http://herschel.esac.esa.int
Identified in the NASA/IPAC Extragalactic Database – http://ned.ipac.caltech.edu/
This material is based upon work at the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261) We gratefully acknowledge support to Exeter from the Leverhulme Trust (F/00144/BJ) and STFC (ST/F0071241/1, ST/H002707/1). This research is partly based on data obtained from the ESO Science Archive Facility, and the CFHT Science Archive. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the Washington Double Star Catalog maintained at the US Naval Observatory. This research has made use of data obtained from the SuperCOSMOS Science Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
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The Taurus Boundary of Stellar/Substellar (TBOSS) Survey — I. Far-IR disk emission measured with Herschel
A&A 570, A29 (2014)
A submillimetre search for cold extended debris disks in the Pictoris moving group
A&A 508, 1057-1065 (2009)
DUst around NEarby Stars. The survey observational results
A DEBRIS disk around the planet hosting M-star GJ 581 spatially resolved with Herschel
AKARI/IRC 18 μm survey of warm debris disks
Astronomy & Astrophysics (A&A)
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The aim of study. To increase the efficiency of reproductive function restoration in women with infertility on the background of thyroid gland pathology, prevent miscarriage, reduce the incidence of gestational complications, improve perinatal outcomes and reduce neonatal morbidity.
Study design. 221 women with infertility on the background of thyroid pathology were examined. Patients were divided into two clinical groups. The group I consisted of 92 women with induced pregnancies (IB) who received pregravid preparation: oral Ogestan® micronutrient complex (potassium iodide in a daily dose of 150 μg, folic acid 400 mg, vitamin D 5 μg, omega-3 fatty acids 200 mg docosahexaenoic acid, vitamin E 12 mg), micronized progesterone (Utrogestan®) 200 mg in the II phase of the menstrual cycle was intravaginal. Group II (129 women) with IB did not receive pregravid preparation.
Results. In the group I 56 women (60.9%) became pregnant after induction of pregnancy, in the group II – 62 women (48.1%). The level of hormones in the serum showed the clinical effectiveness of pregravid preparation according to the method proposed by the authors. Thus, in pregnant women of group I low normal levels of TSH and high normal levels of free T4 were noted, which is a prognostically favorable index for the induction of ovulation. On the levels of progesterone and estradiol in pregnant women of group II, the stress of functioning of the mother-placenta-fetus system was noted, which led to a significantly high frequency of obstetric and perinatal complications. Analysis of the flow of pregnancy and childbirth in the group I showed a significantly lower frequency of a number of complications, which led to a significantly lower frequency of abdominal delivery (64.0%) and neonatal morbidity in the early neonatal period (14.8%).
Conclusion. The inclusion of the Ogestan® complex in the schemes of pregravid preparation of women with infertility on the background of pathology of the thyroid gland is an effective way to replace the deficiency of the most important micronutrients and can be recommended for practical use.
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Hassan, S.S., Romero, R., Vidyadhari, D., et al.; PREGNANT Trial. "Vaginal progesterone reduces the rate of preterm birth in women with a sonographic short cervix: a multicenter, randomized, double-blind, placebo-controlled trial." Ultrasound Obstet Gynecol 38.1 (2011): 18–31.
Zarutskie, P.W., Phillips, J.A. "A meta-analysis of the route of administration of luteal phase support in assisted reproductive technology: vaginal versus intramuscular progesterone." Fertil Steril 92.1 (2009): 163–9.
Vaisbuch, E., De Ziegler, D., Leong, M., et al. "Luteal-phase support in assisted reproduction treatment: real-life practices reported worldwide by an updated website-based survey." Reprod Biomed Online 28.3 (2014): 330–5.
Practice Committee of the American Society for Reproductive Medicine. "Current clinical irrelevance of luteal phase deficiency: a committee opinion." Fertil Steril 103.4 (2015): e27–e32.
Kupka, M.S., Ferraretti, A.P., De Mouzon, J., et al. "European IVF-Monitoring Consortium, for the European Society of Human Reproduction and Embryology Assisted reproductive technology in Europe, 2010: results generated from European registers by ESHRE." Hum Reprod 29.10 (2014): 2099–113.
1. Перминова, С.Г. Бесплодие у женщин с патологией щитовидной железы: принципы диагностики, тактика ведения: автореф. дис. … канд. мед. наук / С. Г. Перминова. – М., 2010. – 34 с.
2. World Health Organization. Guideline: Vitamin D supplementation in pregnant women. World Health Organization (2012).
3. De Groot, L., et al. "Management of thyroid dysfunction during pregnancy and postpartum: An Endocrine Society clinical practice guideline." J Clin Endocrinol Metab 97 (2012): 2543.
4. Hollis, B.W., Johnson, D., Hulsey, T.C., et al. "Vitamin D supplementation during pregnancy: double-blind, randomized clinical trial of safety and effectiveness." J Bone Miner Res 26.12 (2011): 3001.
5. World Health Organization. Fats and Fatty Acids in Human in Nutrition. Joint FAO/WHO Expert Consultation, November 10–24, 2008, Geneva, Switzerland.
6. Wolff, T., Witkop, C.T., Miller, T., Syed, S.B. "Folic acid supplementation for the prevention of neural tube defects: an update of the evidence for the U. S. Preventive Services Task Force." Ann Intern Med 150 (2009): 632.
7. Пустотина, О.А. Роль фолатов в развитии осложнений беременности / О.А. Пустотина, А.Э. Ахмедова // Эффективная фармакотерапия. – 2014. – Вып. 35.
8. Pal Suren, et al. "Association Between Maternal Use of Folic Acid Supplements and Risk of Autism Spectrum Disorders in Children." JAMA 6.309 (2013).
11. Di Renzo, G.C., et al. "Guidelines for the management of spontaneous preterm labour." J Fetal Neonatal Med 24.5 (2011): 659–67.
12. American College of Obstetricians and Gynecologists. "ACOG practice bulletin No. 130: prediction and prevention of preterm birth." Obstet Gynecol 120.4 (2012): 964–73.
13. Preterm Birth Prevention: Evidence-Based Use of Progesterone Treatment Issue Brief and Action Steps for Medicaid Health Plans (2014). Available from: [http://www.mhpa.org/_upload/PTBIssueBrief111714MHPA.pdf].
14. Romero, R., Nicolaides, K., Conde-Agudelo, A., et al. "Vaginal progesterone in women with an asymptomatic sonographic short cervix in the midtrimester decreases preterm delivery and neonatal morbidity: a systematic review and metaanalysis of individual patient data." Am J Obstet Gynecol 206 (2012): e1–19.
15. Cetingoz, E., Cam, C., Sakalli, M., et al. "Progesterone effects on preterm birth in high-risk pregnancies: a randomized placebocontrolled trial." Arch Gynecol Obstet 283 (2011): 423–9.
16. Профилактика невынашивания и преждевременных родов в современном мире. Резолюция Экспертного совета в рамках 16-го Всемирного конгресса по вопросам репродукции человека (Берлин, 18–21 марта 2015 года): Информационное письмо. – М.: Редакция журнала StatusPraesens, 2015. – 4 с.
17. Hassan, S.S., Romero, R., Vidyadhari, D., et al.; PREGNANT Trial. "Vaginal progesterone reduces the rate of preterm birth in women with a sonographic short cervix: a multicenter, randomized, double-blind, placebo-controlled trial." Ultrasound Obstet Gynecol 38.1 (2011): 18–31.
18. Zarutskie, P.W., Phillips, J.A. "A meta-analysis of the route of administration of luteal phase support in assisted reproductive technology: vaginal versus intramuscular progesterone." Fertil Steril 92.1 (2009): 163–9.
19. Vaisbuch, E., De Ziegler, D., Leong, M., et al. "Luteal-phase support in assisted reproduction treatment: real-life practices reported worldwide by an updated website-based survey." Reprod Biomed Online 28.3 (2014): 330–5.
20. Practice Committee of the American Society for Reproductive Medicine. "Current clinical irrelevance of luteal phase deficiency: a committee opinion." Fertil Steril 103.4 (2015): e27–e32.
21. Kupka, M.S., Ferraretti, A.P., De Mouzon, J., et al. "European IVF-Monitoring Consortium, for the European Society of Human Reproduction and Embryology Assisted reproductive technology in Europe, 2010: results generated from European registers by ESHRE." Hum Reprod 29.10 (2014): 2099–113.


text:
Help Takes A Few
N.Y. Times critic Manohla Dargis has trashed The Help, calling it a "big ole slab of honey-glazed hokum." And she's pretty much dismissed every performance in the fiim except for Viola Davis's, which means, I suspect, that unless the entire world disagrees Davis has the heat and Octavia Spencer is out and that's it.
(l. to r.) Emma Stone, Octavia Spencer and Viola Davis in The Help.
Same thing from New York's David Edelstein and Movieline's Stephanie Zacharek: Davis is a solid standout in an overly gauzy, so-so film.
Which is too bad because I feel Spencer's performance is also quite special. She's broad at times but she touches bottom. If you ask me it's her and Davis, her and Davis, her and Davis. Wait…Zacharek to the rescue. "The whole idea of The Help is that a maid isn't just a maid, and Davis and her co-star, Octavia Spencer, breathe life into that idea," she says. "As the quietly crusading Minny, Spencer has some of the movie's best comic moments, though she never lets us lose sight of the justifiable anger and frustration that have come to rule her life."
Davis "keeps her cool even as she warms your heart and does her job, often beautifully," Dargis writes. "She doesn't just turn Aibileen, something of a blur in the novel, into a fully dimensional character, she also helps lift up several weaker performances and invests this cautious, at times bizarrely buoyant, movie with the gravity it frequently seems to want to shrug off."
Edelstein is saying that The Help "belongs to Viola Davis..it's a tough, beautifully judged performance — it gives this too-soft movie a spine."
For what it's worth, The Help isn't doing too badly — 74% — at Rotten Tomatoes so far.
August 9, 2011 11:10 pmby Jeffrey Wells
The Manville Legacy
Some of us can tell right away when we've seen an Oscar-calbre performance. Others can spot this and which category the actor/actress can reasonably be expected to compete in…just like that. If you had to think last year about whether Another Year's Lesley Manville should have run as Best Actress or Best Supporting Actress, you were already behind the eight-ball. It was dead obvious she had to run in as supporting, even with literalists like Coming Soon's Ed Douglas more or less saying that Manville is a lead, the film is mainly about her, her character has the strongest and saddest arc, etc.
Earlier today Cinema Blend's Katey Rich tweeted that The Help's Viola Davis is a Best Actress contender, despite it being thuddingly obvious that the only category Davis can possibly hope to compete in is Best Supporting Actress. (And who decided by the way that Davis is the big Help contender and not Octavia Spencer?) It doesn't matter if Davis's character carries the weight and dignity of the film on her shoulders… which she does. She can't hope to win against Streep/Close. On top of which Davis is "due" so the obvious move is to go for Best Supporting. Case closed, end of story.
Don't Lesley Manville her! Don't Ed Douglas her! Give Davis a fighting chance!
August 9, 2011 5:49 pmby Jeffrey Wells
"Bricks On A Donkey"
I don't care if this interview between Bill Moyers and Oliver Stone is 20 months old. It's the most nourishing and sobering thing that's seeped into my head all day. It's basically Stone talking about his time as an infantryman in Vietnam, and how that experience has informed his views of the current debacle in Afghanistan, and convinced him that Obama has made a terrible mistake by trying to go for some kind of win over there, which of course is futile.
Forget segment #1 — start with segment #2 and then watch segment #3, segment #4 and segment #5.
I don't know what I ought to know about music, so I'm guess I'll be listening to this weekly podcast so I'll have a clue the next time I'm shuffling around Hollywood Ameoba (Sunset and Cahuenga). Co-hosted by the currently untethered Jett Wells and Syracuse U. pally Nathan Matisse, now working in some fringe capacity at Wired. Did Keanu Reeves invent the term "whoa"? No, but he owns it. You can't say it without thinking of him in Bill and Ted's Excellent Adventure.
Muddy Kid
My whole life has been about avoiding and hating films like this, and doing everything I can to persuade others to follow suit. I'd also like to devote my next life to same, even if I come back as a horse or a rabbit or a drop of water in a fountain.
Nothing Recedes Like Success
I'm sure John Wood was extremely grateful when he landed the part of has-been playwright Sidney Bruhl in the stage version of Ira Levin's Deathtrap, which opened in February 1978. For the dryly debonair and deliciously decrepit manner Wood lent to the role was so popular with everyone that he became a major character actor in Hollywood films through the '80s and '90s. The irony is that he never found a part in any Hollywood film that was as much fun to play (or watch) as Sidney Bruhl. Not one. Not even close.
Wood at Dr. Stephen Falken in WarGames.
I know. I caught Deathtrap toward the end of Wood's run (I think) in the late summer or early fall of '78. By that time he'd given so many performances he was going a little batty. He was seized with concentration but also looked half-stoned. "I'm jumping off a proverbial cliff with this part and I don't care because it's so much fun….yaaahhh!," he seemed to be saying. I remember noticing that he was half-muttering his costars' lines — you could almost see his lips move. He was hamming it up for dear life. And when he said "nothing recedes like success" early in the play, he was brilliant. The audience loved him, applauded him. He was so confident, so alive, so cup-runneth-over.
And then the movies let him down. In the '80s, I mean. A couple of minor flashes of flavor but that's all. Somebody Killed Her Husband…forget it. Dr. Stephen Falken in WarGames…gimme a break with that running-around-in-the-cave scene at the end. The thin-lipped Deacon of Diction in Richard Donner's Ladyhawke…blah. All right, he was not only pretty good but fit the tuxedo in Woody Allen's The Purple Rose of Cairo. But then it was back to hell in Jumpin' Jack Flash and then a mini-part in Mike Nichols' Heartburn. And then a supporting role in Lady Jane…okay, not bad.
The the '90s kicked in and Wood started to get a little bit luckier. Archduke Karry in Orlando. A pretty good part in The Madness of King George. And then parts in Uncovered, Sabrina, Richard III, Jane Eyre and so on. And then he got older and started to slow down in the aughts He died in his sleep on 8.6.11.
Wood had been a Shakesperean stage actor for a little less than 30 years before doing Deathtrap, and I'm presuming he was quite content with his work and life during the '50s, '60s and '70s before Levin's play came along. I'm sure his accountant was very happy with Wood's post-Deathtrap income, and I'm sure Wood was pleased as well. If only he could have landed one killer movie role, just one.
(l. to.r.) Wood, Marian Seldes and Victor Garber during the '78 stage production of Deathtrap.
Voicebox
The one thing I didn't like very much about Rise of the Planet of the Apes is Ceasar's unnaturally deep, vaguely creepy voice. This was a concession, I felt, to a basic Hollywood notion that formidable warrior figures have to sound snarly and tough and commanding in some primal way. But if you've seen footage of a talking ape (as I have) you know they don't have deep, dark voices but ones that are on the soft, high-pitched side. They sound like very old white men. So while the line "Ceasar is home" worked, the delivery didn't.
August 9, 2011 11:48 amby Jeffrey Wells
Reports about Anne Hathaway's stunt double having driven her Catwoman chopper right into an IMAX camera yesterday (i.e., Monday) on the set of The Dark Knight Rises don't say if the camera was totalled or partly damaged or what. The TMZ Video shows the bike hitting the camera at a relatively slow speed, and that some of the damage (whatever it amounts to) will be from the IMAX camera having been dropped by the cameraman.
What does an IMAX camera cost? $350,000? A half million? Even if was completely destroyed (which I doubt), keep two things in mind: (1) There's a mention on The Dark Knight's iMDB page that "while filming [a] chase scene with the Joker and the SWAT vans, one of only four IMAX cameras in the world at that time was destroyed." And (2) this pales compared to the 1958 incident on the set of Ben-Hur when a $100,000 65mm camera was totally destroyed during the filming of the chariot race. The Dollartimes inflation converter says a 1958 dollar would be worth $7.72 in 2011, so the smashed Ben-Hur camera cost filmmakers the equivalent of $772,000.
August 9, 2011 8:02 amby Jeffrey Wells
Base Is Freaking
The same basic despair expressed by my recent "Hillary Should Have Won" riff was concurrently written and reported about by The Daily Beast's Leslie Bennetts. "During the last few days, the whispers have swelled to an angry chorus of frustration about [President] Obama's perceived weaknesses," she wrote. "Many Democrats are furious and heartbroken at how ineffectual he seemed in dealing with Republican opponents over the debt ceiling, and liberals are particularly incensed by what they see as his capitulation to conservatives on fundamental liberal principles."
The American middle-classes have never and will never take to the streets to vent anger about anything, ever. Despair and quiet grumbling and prescription drugs is as far as it goes over here. But wouldn't it feel…well, therapeutic on some level if something could happen in the streets of the U.S. of A. that would express basic fundamental rage about how the corporate elites are turning (have turned?) this country into South America, and how the radical legislative right has gone completely insane, etc.?
I know what's going on in England right now — young have-nots are enraged at drastic cuts in social spending by David Cameron's conservative government. It's obviously a vastly different picture and climate, but this country so needs to get mad, mad, Peter Finch-mad.

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text:
Court Acquits Journalist Jarkloh of Rape, Sodomy Charges
... Nolle Prosequoi Filed
06/10/08 - FPA Staff Report
Monrovia -
Prosecuting lawyers for the Liberian government in the Rape case - Bill Jarkloh Vs. Republic of Liberia - have entered a Plea Of "Nolle Prosequoi" thus clearing Journalist Bill Jarkloh all the charges of rape and sodomy brought against him recently by the family of a 8 years old child.
The Plea Of "Nolle Prosequoi" followed journalist Jarkloh pleaded for his temporary release from prison based on the lack of sufficient evidence to prosecute him.
Free for now: Journalist Bill Jarkloh
On May 13, Journalist Jarkloh was issued a writ of arrest by the Monrovia City Court for allegedly committing rape and sodomy as was claimed by mother of an eight-year old girl, Janjay who said the crime took place at Bill's Perry Street residence.
However, such plea allows prosecution the time to reserve the right to re-file the case should the need arise in keeping with section 18.1 of the Criminal Procedure Law. The Assistant County Attorney, Witness Doyen, last Friday filed a plea of "nolle prosequoi" without prejudice before the Monrovia City Court at the Temple of Justice after the case had been scheduled for preliminary hearings on the same day.
A nolle prosequi may be entered either in a criminal or a civil case. In criminal cases, a nolle prosequi may be entered at any time before the finding of the grand jury, and generally after a true bill has been found. No nolle prosequi can also be entered after a bill has been found, without leave of the court, except in cases of assault and battery, fornication and bastardy, on agreement between the parties, or in prosecutions for keeping tippling houses.
A nolle prosequi may be entered as to one or several defendants. The effect of a nolle prosequi, when obtained, is to release the defendant without day, but it does not operate as an acquittal; for he may be afterwards reindicted, and even upon the same indictment, fresh process may be awarded.
Journalist Jarkloh had since expressed his innocence but family members of the survivor are still protesting that the minor did identify Bill as the doer of the crime. Hearings into the case had been experiencing hitches since it was first issued a notice of assignment which was scheduled by the court on May 27, 2008 due to what the defense lawyer cited as no police charge sheet' to serve as the court's document that should indict the accused.
Meanwhile, according to the law, a case wherein the proof is not evident and presumption is not grave, the suspect can be set free either on bail or the prosecution can nolle prosequoi the case, requesting time to gather all evidence thereby evoking section 18.1 of the criminal procedure law.
No conclusion yet, prosecutors say
But for the case of rape which is nonbaillable, prosecution says such plea gives them the right to request for time so as to inquire from the police regarding the report of the full scale investigation earlier conducted into Bill's case. Police has already reported to state prosecutors with the name of Journalist Jarkloh mentioned nowhere in it. It instead linked one Lincoln who ploice quoted Love as saying raped her in a video club in the night.
Prosecution further said that the case has not yetreached its conclusion therefore they have advised the aggrieved party to appear today to continue the process of first establishing who the suspect is and to sort out other new evidence if possible.
The case was issued a notice of assignment over four times by the Monrovia City Court under the gavel of Associate Magistrate Wondah Sondah but because of the court's failure to begin said hearings, the defense prayed that the case be transferred to an upper court that has similar jurisdiction over said matters.
The case was turned over to Court "B" under the gavel of Judge Evelyna Quaqua who also scheduled the case for last Friday at which time she was expected to give ruling since the prosecution had earlier informed the City Court that there was no sufficient court document to prosecute the case.
But to the dismay of both parties, the Court 'B' Judge could not appear at the time set to call the case while the parties waited in the court room. When reporters engaged her in her chambers, she told them that she had decided to reserve her ruling due to her personal judgment which is in the interest of both parties and that she was awaiting orders.
The defense lawyer, apparently, out of patience that his client would have spent another weekend in prison based on Judge Quaqua's decision returned the case to the City Court where prosecution was granted the right to evoke section 18.1 of the Criminal Procedure Law.
Meanwhile, Jarkloh, since his release from prison has continued to profess his innocence of the charges.
Maintaining innocence
"The fact remains that "I am innocent, and I am being humiliated by a conspiracy masterminded and championed by Sorbor George", a reporter of Star Radio in Monrovia. Mr. George and I lived in the same building but in separate apartments. Besides, he said, "the conspiracy against him is also being masterminded by officials of the court," Jarkloh told FrontPageAfrica Tuesday.
Jarkloh says that the Magistrate was instructed by someone at the helm of power, the Chief Justice of Liberia, to deny him and his fiancée Korpo S. Kortimai, a daughter of former deputy Commerce Minister Professor Lavela B. Kortimai bail because "he and enemies of progress want Korpo and I to be brought to the South Beach together disgraced for a good we did. But God says "the truth that is buried shall rise again," Jarkloh added.
Jarkloh says the crux of the matter is that one Janjay, said to be a mother of eight-year-old "Tenesee" (Love) Samuels abandoned Love for more than one month and chased her out of their residence. "This minor was sleeping in street corners, video clubs and under market stalls. Love told Korpo, human right activist/personnel, how one Lincoln had abused her at a video club in the middle of the night."
Thereafter, he said, a lady rescued her and turned her over to Korpo as people in the community usually do when an abandoned or abused child was found. "Korpo Kortimai, as usual, took "Love" to Love's "mother" Janjay but Janjay told Korpo that because she Janjay didn't want Love to run from the house again, (Korpo) should keep the child and counsel her. But looking at the poor health situation, Korpo had reported this minor to the Women and Children Protection Unit of the LNP (Central). Love was processed at the police Headquarters and taken to a "Safe Home," Jarkloh says. But a week later, according to Jarkloh, Janjay started to grumble Korpo to see the "Safe Home", apparently thinking that sending Love there is for pecuniary gain to Korpo and her household. And because there are already envious people in the community that Korpo and I live, they have now connived; saying that my charming spouse, Korpo, "kidnapped" Love while I raped and sodomized the little girl.
Jarkloh alleges that the police investigation regarding the abandonment and raping of Love was ignored for whatsoever interest to order the issuance of a writ of arrest against him for "SODOMY/RAPE" without a police charge sheet; at the same time, warning Attorney Doyen who is insisting on outcome of police investigation to keep off the matter. "Instead, Justice Johnnie Lewis said he preferred Attorney Sam T. Solomon to use Janjay and my enemies to incarcerate me at the Monrovia Central Prison (South Beach) without the police report on the case and medical documents (report) to establish their claims against me."
Looking back on the ordeal, Jarkloh laments that a good deed turned into a personal tragedy. "My fiancée and I have been good to Love and her mother. Unfortunately, our kindness has turned into bad and we are being paid with false charges just to destroy our hard earned reputation and characters."


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The disciples Jesus called did forsake all/ they walked away from their Family, and their Jobs, and their Business, when he called/ As to What the gain was, it was JESUS/!!!
PONDER THE REAL WORDS OF JESUS/ PONDER the IMPLICATIONS of these WORDS?
(Luke 9:23) And he said to all, "If anyone would come after me, let him deny himself and take up his cross daily and follow me.
KEY WORD IS DENY SELF/ self is always about you, Denying Self is Following JESUS.
I had been Pondering many things about Jesus and his life, and all at once these things I had been thinking about where all put together, and expounded upon by the Holy Spirit.
Then many people seem to be lacking in knowledge as to how Hebrews brought up their Sons/ Schooling etc, hasn't changed much in 2,000 years/ So there are No Lost Years of JESUS, he was doing what most Hebrew sons do/ Studying the torah, being schooled, etc. How else would he have been called a RABBI???
We have Angels speaking to Mary and Joseph on several occasions, but to think that they where left to raise the Son of God on their own is unrealistic/ Iam sure that they where instructed many, many times on what to do to raise the Son of God, throughout Jesus life Time.
It is also clear that Jesus's Mother was familiar with his ability to do miracles/ so he would have been doing this for sometime/ LONG before the Wedding where he did his First PUBLIC Miracle.
But as soon as this happens, then JESUS begins to embark on his Journey to the Cross.
(Matthew 16:24; Mark 8:34; Luke 9:23)?"
To a person in the first-century, the cross meant one thing and one thing only: death by the most painful and humiliating means human beings could develop.
JESUS came to TAKE CARE of us All/ He took on the Responsibility of Supplying the needs of everyone.
That is what he did throughout his Whole Life/ He took care of everyones needs, wherever he went.
Take up your cross and follow Me" It is a Calling to SERVE the NEEDS of others, and leave your own behind.
Every day JESUS got up and went about Ministering to those who where Sick, and Oppressed/ He taught in crowds, and he went one on one to peoples houses to Make a House call to Heal them.
This is what all those who are Calling themselves followers of Christ are suppose to be doing/ But this is not what is actually happening, since most of the so called followings are looking to be SERVED.
Supplying your Needs is what JESUS does/ THAT IS HIS PURPOSE/ so how can you not have FAITH in him doing what he was SENT TO DO/ Be your CARE TAKER.
JESUS was Hanging on the Cross Dying, when he performs his Last Responsibility/ Here is JESUS Dying, while thinking of his own MOTHER, and how he wants her taken care of/ when he is gone.
This is the ULTIMATE EXAMPLE of Selflessness/ Thinking of others while you are Dying/ not to mention MULTI DIMENSIONALLY changing Reality/ Our God is always in more then One Place at a time.
If Jesus Prepared away to take care of his Family before he was Born, If he Prepared away to Take Care of his own Mother while Dying, if he can feed 5000 people lunch/ If he can take away the Sin of the World, Then how can you Doubt that he will always TAKE CARE OF YOU?
shall be last of all, and servant of all.
WHO ARE YOU SERVING? WHO ARE YOU TAKING CARE OF?


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text:
Iraqi journalists stage protest
Hundreds of people demonstrate in Baghdad against "censorship and intimidation".
Journalists have complained about a government
plan to restrict some websites [EPA]
"Journalists and media workers have lost 247 of their colleagues over the past six years because of attacks and violations," Emad al-Khafaji, a journalist and writer, told the crowd on Friday.
"The participants in this demonstration have confirmed they will not back down in the face of intimidation and threats."
Website ban considered
Journalists are also concerned about government moves to ban some websites, including those deemed pornographic or to encourage bomb making, prostitution and "terrorism".
Last month, the government passed a bill allowing imported publications to be screened.
"Blocking internet websites and censoring books is a new dictatorship," Muhammad al-Rubaie, a human rights activist at the demonstration, said.
The crowd at Friday's protest, who carried signs saying "do not kill the truth", shouted: "Yes, yes to freedom; no, no to being muzzled".
The Iraqi constitution, which was drawn up in 2005, enshrines freedom of the press and publication unless "public order or morality" is violated.
Ahmed Rushdi, an Iraqi journalist, told Al Jazeera that the government was considering laws to "capture and control any data broadcast, published or uploaded from Iraq".
"This is not acceptable, this is an error in the constitution ... we'll not accept any capturing, we will not accept any silencing, I will not accept to break my pen for [the prime minister] Maliki's sake or any other government," he said.
"Before 2003 there was such silencing, now there will be no silencing."
Under Saddam Hussein, the deposed Iraqi president, the media was heavily censored.
Since the US-led invasion in 2003 that led to Hussein's removal from power, about 200 print outlets, 60 radio stations and 30 television channels have been set up.
But many media outlets are dominated by sectarian and party patrons who use them to push their own agendas.


In the list of top 10 construction companies in USA, all the companies have millions of turnover every year. Each company has over thousands of labours, workers, staffs and engineers including all. These top 10 construction companies in USA has been also completed many projects of USA as well as in the world. Many of them have the branch offices in across various countries. The list of the construction companies in USA is not least. However, in this post, we will only have the top construction companies in USA. So, the journey of the construction companies in USA is good. They have been assigned many projects and finished the projects successfully.
The career and future in the list of top 10 construction companies in USA are really bright. As these companies are serving services more than a century. The top 10 construction companies are founded in early 19's. Well, some of the top 10 construction companies in USA are recognised as the Fortune 500. You can also look into our post i.e. Top 10 Construction Companies In India.
The journey of this company was started from Sydney, Australia. But now this company becomes one of the top 10 construction companies in USA. Their regional head offices are located in New York, Singapore, and London. Lendlease has approximately 12,000 employees internationally.
In 1970, operations expand to the US and in 1999, Lend Lease acquires Bovis, P&O's project management company. Lend Lease delivers the US' first LEED Gold Certified building in 2003. It is world's largest construction company.They have secured major urban regeneration projects such as Barangaroo South, Darling Square, Victoria Harbour and Brisbane Showgrounds in Australia; Elephant & Castle and International Quarter London in the United Kingdom; Paya Lebar Quarter and Tun Razak Exchange in Asia; and Riverline in the United States.
The J.A. Jones Inc was founded in 1890's by James Addison Jone. It is one of the oldest construction companies from the listing of top 10 construction companies in USA. J.A. Jones Construction assisted in the building of the Petronas Towers in Malaysia. However, the company headquartered in Charlotte, North Carolina.
The company Halliburton is much famous and renowned for its oil field services in approximately 70 countries. This company has approximately 50,000 members who worked for the development of this company including workers, staffs, engineers, experts, etc.
The company has dual headquarter i.e. located in Houston and in Dubai. The company is listed under top 10 construction companies in USA and it is the world's largest oil field services. The company serves the upstream oil and gas industry throughout the lifecycle of the reservoir – from locating hydrocarbons and managing geological data, to drilling and formation evaluation, well construction, completion, and production optimization.
5. Peter Kiewit Sons, Inc.
The company was founded in 1884. It one of the oldest company in the top construction companies in USA. Kiewit is one of North America's largest and most respected construction and engineering organizations. The employee-owned company operates through a network of offices and projects in the United States, Canada, and Australia. Nearly all construction projects are staffed by one or more owners of our company.
Bruce Grewcock, Kiewit's CEO, has steered the company to excellence since 2004. He is only the fifth person to assume leadership of the company in its modern era. Peter Kiewit, Bob Wilson, Walter Scott Jr., and Ken Stinson preceded him. In 2012, in addition to his CEO responsibilities, Grewcock was named the chairman of the board.
According to the company official statement in about us page they described as Skanska is one of the world's leading project development and construction groups, concentrated on selected home markets in the Nordic countries, other European countries and in North America. With a focus on sustainability, we offer competitive solutions – not least for the most complex assignments.
The company was founded in 1902, founded by Henry C. Turner. Turner is a North America-based, international construction services company and is a leading builder in diverse market segments. The company has earned recognition for undertaking large, complex projects, fostering innovation, embracing emerging technologies, and making a difference for their clients, employees, and community.
Consistently ranked among the nation's largest building contractors, Balfour Beatty Construction Services US has been cited as a Top 10 Domestic Building Contractor and Top 10 Green Builder by Engineering News-Record. It was founded in 1933. The company provides large quality services of Construction Management, General Contracting, Cost Consulting, Design-Build, Preconstruction Services, Public-Private Partnerships.
Centex Construction (founded in 1950) is acquired by Balfour Beatty, plc to form Balfour Beatty Construction (BBC) in the U.S.
Flour Corporation is the largest engineering & construction company in the Fortune 500 rankings and lists 136th overall in the same rankings. It is one of the best conruction company among the top 10 construction companies in USA. The company delivers integrated engineering, procurement, fabrication, construction (EPFC), maintenance and project management solutions to governments and private sector Clients in diverse industries around the world. Fluor develops and implements innovative solutions for complex project issues. For over a century, Clients selected Fluor as their company of choice to complete challenging projects in remote parts of the world. The company was founded in 1912.
According to its official website, they described the companies as Bechtel is one of the most respected global engineering, construction, and project management companies. Together with their customers, we deliver landmark projects that create long-term progress and economic growth.
Since 1898, they've completed more than 25,000 extraordinary projects across 160 countries on all seven continents. They operate through four global businesses: Infrastructure; Nuclear, Security & Environmental; Oil, Gas & Chemicals; and Mining & Metals. Their company and our culture are built on more than a century of leadership and a relentless adherence to our values, the core of which are safety, quality, ethics, and integrity. These values are what they believe, what they expect, what they deliver, and what they live. It is also one of the oldest construction company among the top 10 construction companies in USA.