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Ward, J N, 5394
No full textThis record was harvested from a previous catalogue system and will be withdrawn in 2025. Information in this record may be superseded or incomplete. Visit this record in UMA's new catalogue at: https://archives.library.unimelb.edu.au/nodes/view/423896Surname: WARD. Given Name(s) or Initials: J N. Military Service Number or Last Known Location: 5394. Missing, Wounded and Prisoner of War Enquiry Card Index Number: 9980.251532
Item: [2016.0049.56157] "Ward, J N, 5394
Summary of LCO 5394
No full text"May 1, 2012."; Discusses LCO 4231 (HB 5394--an Act Concerning Smoke and Carbon Monoxide Detectors and Alarms in Residential Buildings).; Harvested from the web on 5/7/1
CO observations of the interacting galaxy pair NGC 5394/95
No full textBIMA 12CO J = 1 → 0 observations are presented of the spiral galaxies NGC 5394 and NGC 5395 that have undergone a recent, grazing encounter. In NGC 5394 approximately 80% of the CO emission detected by BIMA is concentrated in the central 800 pc (FWHM) starburst region, and the rest is from a portion of the inner disk south and west of the central starburst. In an encounter simulation that reproduces some of the main features of this galaxy pair, a considerable amount of gas in NGC 5394 falls into the central region early in the collision. The observed total gas distribution in the disk of NGC 5394 is lopsided, with more H I, CO, and Hα emission coming from the western or southwestern side. The innermost western arm of NGC 5394 is seen in CO and Hα emission, but the eastern inner-disk arm, which is very bright in the optical continuum, is not detected in CO or Hα emission. The NGC 5394 starburst region is similar in radio continuum luminosity and size to the M82 starburst and has a CO luminosity ∼4 times greater. A CO position-velocity diagram of the NGC 5394 nucleus reveals two separate velocity features very close to the center. This may indicate a nuclear ring or the "twin peaks" of an ILR or some depletion of 12CO J = 1 → 0 at the nucleus. From a comparison of the radio continuum, Hα, 60 μm, and CO luminosities, we estimate that the average extinction A v of the starburst nucleus is 3-4 mag, the star formation rate is ∼6 M⊙ yr-1, and the conversion factor N(H 2)/ICO in the starburst is a factor of 3-4 below the standard value. Comparison of NGC 5394 with two other systems previously studied suggests that in prograde grazing encounters a central starburst may not develop until near the end of the ocular phase. Very little of the CO emission from NGC 5395 found in previous single-dish observations is detected in the BIMA data; thus molecular gas in NGC 5395 does not appear to be strongly concentrated in compressed ridges
[Carolina Clinchfield & Ohio, Engine Drawing Card, Sketch No. 5394]
No full textThis engine drawing card was created for Carolina Clinchfield & Ohio Railway, Class 20 46/74 EE. Section J-20 1/4 EE. Sketch 5394. Copy Spec. B4331
Interaction Between NGC 5394 and NGC 5395
Get PDFThe spiral galaxies NGC 5394/95 (at a distance of 47 Mpc) are involved in a recent, close, nonmerging encounter. The smaller galaxy, NGC 5394, has two long, fairly symmetric, open tidal arms (see Figure 1); in numerical simulations, this type of structure results from a close, prograde, nearly in-plane encounter. To study this galaxy pair, we used the VLA to obtain HI (21 cm line) and radio continuum data, the Maryland-Caltech Fabry-Perot camera to obtain Ha data, the 2.1m telescope at KPNO, the Fick observatory 0.6 m telescope, and the Burrell-Schmidt telescope to take optical and near-infrared images, and Onsala Space Observatory for CO J=1-0 observations
Summary of eminent domain amendment (LCO 5394) to sSB 34
No full textElectronic data.; Title from Web page (viewed May 16, 2006).; "May 1, 2006."; Provides a section-by-section analysis of LCO 5394, amending sSB 34 regarding eminent domain.; Harvested from the web on 5/17/0
The Interacting Galaxies NGC 5394/5395: A Post-Ocular Galaxy and Its Ring/Spiral Companion
No full textH I, radio continuum, Fabry-Perot Hα, and 12CO J = 1 → 0 observations and broadband optical and near infrared images are presented of the interacting spiral galaxies NGC 5395 and NGC 5394. Kinematically, there are three important, separate components to the H I gas associated with this galaxy pair: (1) the main disk of NGC 5395, (2) a long, northern tidal arm of NGC 5395 distinct in velocity from its main disk, and (3) the disk of NGC 5394. The H I northern tidal arm of NGC 5395 has a line of–sight velocity as much as 75–100 km s-1 greater than the main disk of NGC 5395 at the same projected location and thus is not in the same plane as the disk. The velocity field of the disk of NGC 5395 is asymmetric and distorted by large-scale and small-scale noncircular motions. In NGC 5395, the encounter appears to be exciting m = 1 and m = 0 modes in what had been a two-armed spiral. The dominant spiral arm of NGC 5395 forms a large ring or pseudo-ring of Hα, radio continuum, and H I emission, somewhat off center with respect to the nucleus. The H I trough in the center of NGC 5395 is not filled in by molecular gas. The Hα velocity contours exhibit an organized pattern of kinks in crossing the ring and also show streaming motions in a large stellar caustic feature. The eastern side of the ring is brighter in radio continuum and Hα; the western side is brighter in H I and contains massive (108 M☉) H I clouds not associated with the most luminous H II regions. The smaller galaxy NGC 5394 is in an immediate post-ocular phase, with a central starburst, an intrinsically oval disk, two long, fairly symmetric, open tidal arms with high arm-interarm contrast, and very bright inner spiral arms, disjoint from the outer tidal arms. Most of the gas in NGC 5394 is in molecular form and concentrated within 3.8 kpc of the center, so is suitable for fueling the starburst. Despite the presence of H I gas, two of the three optically bright inner spiral arms of NGC 5394 show no evidence of ongoing star formation.
A galaxy encounter simulation reproduces some of the main features of this system with a collision that is prograde relative to NGC 5394 and retrograde at a high tilt angle relative to NGC 5395. The model finds that the inner spiral structure of NGC 5394 developed from an eye-shaped ("ocular") structure at slightly earlier times. NGC 5394 and the two ocular galaxies IC 2163 and NGC 2535, studied earlier, form an evolutionary sequence of structures resulting from prograde encounters and thus confirm the generic models of such collisions. The agreement between the model for NGC 5394/95 and the ring/spiral structures seen in NGC 5395 extends our understanding of collisional ring galaxies
The Interacting Galaxy Pair NGC 5394/95: Near-Infrared Photometry, Structure, and Morphology
No full textInternational audienceWe present near-infrared observations in the J, H, and K' passbands of the interacting pair of galaxies NGC 5394/95 (KPG 404). The total magnitudes, colors, surface brightnesses, and color profiles are calculated. In addition, aperture magnitudes are compared against previous determinations. We also perform a structural (disk + bulge) analysis, as well as a two-dimensional Fourier analysis, to gain insight into the morphology of the pair. The disk + bulge fit shows that NGC 5394 (KPG 404A) is more compact than normal galaxies, while NGC 5395 (KPG 404B) is less concentrated. The two-dimensional Fourier analysis shows that NGC 5394 is an H2beta galaxy in the dust-penetrated (DP) classification by Block & Puerari. NGC 5395, in contrast, displays a very complex structure that needs a number of Fourier coefficients to be explained. A tightly wound m=1 coefficient (DP class H1alpha) is the main structure, but other m=1 and m=2 coefficients (suggesting modulation) are also present in the Fourier spectra. The m=1 coefficients represent a pseudo-ring-type structure, indicative of a collision rather than a passage. Based on our results we are able to assert that the scenario of the interaction between the galaxy members of KPG 404 should take into account a crossing of NGC 5394 through the disk of NGC 5395 in a Cartwheel-like encounter rather than a passage as in M51-type pairs. Numerical simulations could help to unravel the structural and morphological evolution of this interacting pair
Going Beyond Counting First Authors in Author Co-citation Analysis
Get PDFThe present study examines one of the fundamental aspects of author co-citation analysis (ACA) - the way co-citation
counts are defined. Co-citation counting provides the data on which all subsequent statistical analyses and mappings
are based, and we compare ACA results based on two different types of co-citation counting - the traditional type that
only counts the first one among a cited work's authors on the one hand and a non-traditional type that takes into
account the first 5 authors of a cited work on the other hand. Results indicate that the picture produced through this non-traditional author co-citation counting contains more coherent author groups and is therefore considerably clearer. However, this picture represents fewer specialties in the research field being studied than that produced through the traditional first-author co-citation counting when the same number of top-ranked authors is selected and analyzed. Reasons for these effects are discussed
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