Optimum earth re-entry corridors

Steepest ascent optimization procedure for reentry trajectory of manned aerospace vehicle

Shocks and Bubbles in a Deep Chandra Observation of the Cooling Flow Cluster Abell 2052

We present results from a deep Chandra observation of Abell 2052. A2052 is a bright, nearby, cooling flow cluster, at a redshift of z=0.035. Concentric surface brightness discontinuities are revealed in the cluster center, and these features are consistent with shocks driven by the AGN, both with Mach numbers of approximately 1.2. The southern cavity in A2052 now appears to be split into two cavities with the southernmost cavity likely representing a ghost bubble from earlier radio activity. There also appears to be a ghost bubble present to the NW of the cluster center. The cycle time measured for the radio source is approximately 2 x 10^7 yr using either the shock separation or the rise time of the bubbles. The energy deposited by the radio source, including a combination of direct shock heating and heating by buoyantly rising bubbles inflated by the AGN, can offset the cooling in the core of the cluster.Comment: accepted for publication in The Astrophysical Journal Letter

The EFIGI catalogue of 4458 nearby galaxies with morphology II. Statistical properties along the Hubble sequence

The EFIGI catalogue of 4458 galaxies provides a reference database of the morphological properties of nearby galaxies, with 16 shape attributes describing their various dynamical components, their texture and environment, and with a dense sampling of all Hubble types. This catalogue allows us to derive a quantitative description of the Hubble Sequence in terms of the specific morphological features of the various types. The variations of the EFIGI morphological attributes with type confirm that the visual Hubble sequence is a decreasing sequence of bulge-to-total ratio and an increasing sequence of disk contribution to the total flux. There is nevertheless a large dispersion of approximately 5 types for a given bulge-to-total ratio, due to the fact that the Hubble sequence is primarily based on the strength and pitch angle of the spiral arms, independently from the bulge-to-total ratio. The grand spiral design is also related to a steep decrease in visible dust from types Sb to Sbc-Sc. In contrast, the scattered and giant HII regions show different strength variation patterns; hence, they do not appear to directly participate in the establishment of the Hubble sequence. The distortions from a symmetric profile also incidentally increase along the sequence. Bars and inner rings are frequent and occur in 41% and 25% of disk galaxies resp. Outer rings are twice less frequent than inner rings, and outer pseudo-rings occur in 11% of barred galaxies. Finally, we find a smooth decrease in mean surface brightness and intrinsic size along the Hubble sequence. The largest galaxies are cD, Ellipticals and Sab-Sbc spirals, whereas Sd and later spirals are nearly twice smaller. S0 are intermediate in size, and Im, cE and dE are confirmed as small objects. Dwarf spiral galaxies of type Sa to Scd are rare in the EFIGI catalogue, we only find 2 such objects.Comment: Accepted for publication in Astronomy and Astrophysics, 22 pages, 10 tables, 19 colour figures. Data available at http://www.efigi.or

Ca II and Na I Quasar Absorption-Line Systems in an Emission-Selected Sample of SDSS DR7 Galaxy/Quasar Projections: I. Sample Selection

The aim of this project is to identify low-redshift host galaxies of quasar absorption-line systems by selecting galaxies which are seen in projection onto quasar sightlines. To this end, we use the Seventh Data Release of the Sloan Digital Sky Survey (SDSS-DR7) to construct a parent sample of 97489 galaxy/quasar projections at impact parameters of up to 100 kpc to the foreground galaxy. We then search the quasar spectra for absorption line systems of Ca II and Na I within +- 500 km/s of the galaxy's velocity. This yields 92 Ca II and 16 Na I absorption systems. We find that most of the Ca II and Na I systems are sightlines through the Galactic disk, through High Velocity Cloud complexes in our halo, or Virgo cluster sightlines. Placing constraints on the absorption line rest equivalent width significance (>=3.0 sigma), the Local Standard of Rest velocity along the sightline (>= 345 km/s), and the ratio of the impact parameter to the galaxy optical radius (<=5.0), we identify 4 absorption line systems that are associated with low-redshift galaxies at high confidence, consisting of two Ca II systems (one of which also shows Na I), and two Na I systems. These 4 systems arise in blue, L_r^* galaxies. Tables of the 108 absorption systems are provided to facilitate future follow up.Comment: 13 pages, 11 figures, 6 tables; online data included in electronic version as 1 FITS table and 2 machine readable tables; to be published in The Astronomical Journa

Reading-to-learn from subject-matter texts: A digital storytelling circle approach

Digital storytelling circles (DSCs) are multimodal platforms aimed at improving students’ comprehension of subject matter texts. In a small group, students in a DSC engage in reading, writing, speaking, listening, viewing, using digital tools, and manipulating texts and instructional strategies. Roles are assigned to each group member as they use the tools provided by the multimodal platform to create a digital story. Most of the literature supports the notion that the experience of creating digital stories can have a positive impact on students’ acquisition of literacy skills and their motivation to engage with the text. This chapter presents a model for using DSCs in the post-reading phase of a Directed Reading Activity (DRA). Case study findings highlight two DSCs that exhibited qualities of developing the literacy strategies necessary in reading-to-learn with complex content area texts.https://nsuworks.nova.edu/fse_facbooks/1000/thumbnail.jp