Immigrant Homebuyers in Lawrence and Lowell, Massachusetts: Keys to the Revitalization of the Cities

This report describes the homebuying experience of immigrants in Lawrence and Lowell, Massachusetts and how it contributes to their lives and the life of the cities. Home ownership provides wealth to individuals and families. As a key financial resource, owning a home provides opportunities to secure the "good life" including education, business, training, health and comfort. As such, successive waves of immigrants in local communities have regarded the eventual acquisition of their first home as a major goal. In so doing, large segments of immigrants have morphed from renters to homeowners. In such instances, we often witness the transitioning of a poor community to one that is working-class emerging to a middle-class. This report is an in-depth description of such a metamorphous among immigrants in Lawrence and Lowell. The study reveals important contributions that immigrants homebuyers have made to the growth and economic health of the two cities

Unsteady Effects in Flow Rate Measurement at the Entrance of a Pipe

Unsteady flow in pipes and nozzles occur frequently in engineering applications and they pose special problems of measurement and calibration. When the Reynolds number is high the entrance region of a pipe (following a smooth contraction) is characterized by a thin boundary layer and the unsteady effects are then bound up in the unsteady behavior of the boundary layer. Woblesse and Farrell [1]2 have recently considered unsteady effects in laminar pipe entrance flows that start from rest by an integral method. Periodic disturbances also arise which require a different treatment. The primary interest of the present work is for thin entrance boundary layers subject to peridodic disturbances. In either case the ratio of the average velocity to the velocity in the potential core is V[sub]avg/V[sub]core = 1- 2[delta]*/R [equation 1] where [delta]* is the usual displacement thickness and R is the pipe radius. In steady flow this ratio is just the "discharge coefficient", c[sub]d. In unsteady flow it is very desirable to know how this ratio changes with time because many of the presently available experimental methods enable one to measure V[sub]core but not V[sub]avg readily. In this brief note we will estimate the unsteady effects of a periodic, fluctuating main flow on the displacement thickness of a laminar, flat plate boundary layer. It is assumed that the boundary layer is sufficiently thin compared to the radius of a pipe so that the pressure gradient caused by this effect in a pipe can be neglected; the results should then be directly applicable to equation (I)

Book Review: Khrist Bhakta Movement: A Model for an Indian Church? Inculturation in the Area of Community Building

Book review of Khrist Bhakta Movement: A Model for an Indian Church? Inculturation in the Area of Community Building. By Ciril J. Kuttiyanikkal. Berlin: LIT Verlag, 2014, 377 pages

Neutral Hydrogen 21cm Absorption at Redshift 0.673 towards 1504+377

We detect the 21 cm line of neutral hydrogen in absorption at a redshift of 0.673 towards the 1 Jy radio source 1504+377. The 1504+377 radio source is located toward the center of what appears to be an inclined disk galaxy at z = 0.674. The 21 cm absorption line shows multiple velocity components over a velocity range of about 100 km sec$^{-1}$, with a total HI column density: N(HI) = $3.8\times10^{19}\times({{T_s}\over{f}})$ cm$^{-2}$. The velocity-integrated optical depth of this system is the largest yet seen for redshifted HI 21 cm absorption line systems (Carilli 1995). The 21 cm absorption line is coincident in redshift with a previously detected broad molecular absorption line system (Wiklind and Combes 1996). We do not detect HI 21 cm absorption associated with the narrow molecular absorption line system at z = 0.67150, nor do we detect absorption at these redshifts by the 18 cm lines of OH, nor by the 2 cm transition of H$_2$CO. There is no evidence for a bright optical AGN in 1504+377, suggesting significant obscuration through the disk -- a hypothesis supported by the strong absorption observed. The 1504+377 system resembles the ``red quasar'' PKS 1413+135, which has been modeled as a optically obscured AGN with a very young radio jet in the center of a gas rich disk galaxy (Perlman et al. 1996). The presence of very bright radio jets at the centers of these two disk galaxies presents a challenge to unification schemes for extragalactic radio sources and to models for the formation of radio loud AGN.Comment: 17 pages, postscrip

Adaptive Information Cluster at Dublin City University

The Adaptive Information Cluster (AIC) is a collaboration between Dublin City University and University College Dublin, and in the AIC at DCU, we investigate and develop as one stream of our research activities, various content analysis tools that can automatically index and structure video information. This includes movies or CCTV footage and the motivation is to support useful searching and browsing features for the envisaged end-users of such systems. We bring in the HCI perspective to this highly-technically-oriented research by brainstorming, generating scenarios, sketching and prototyping the user-interfaces to the resulting video retrieval systems we develop, and we conduct usability studies to better understand the usage and opinions of such systems so as to guide the future direction of our technological research

A legacy handbook for physical regeneration

Legacy Handbook reviewing emda's experience of regeneration activity. Identifies key achievements and draws out lessons learned that may be relevant to successor bodies active in this area

Remnant gas in evolved circumstellar disks: Herschel PACS observations of 10-100 Myr old disk systems

We present Herschel PACS spectroscopy of the [OI] 63 micron gas-line for three circumstellar disk systems showing signs of significant disk evolution and/or planet formation: HR 8799, HD 377 and RX J1852.3-3700. [OI] is undetected toward HR 8799 and HD 377 with 3 sigma upper limits of 6.8 x 10^-18 W m^-2 and 9.9 x 10^-18 W m^-2 respectively. We find an [OI] detection for RX J1852.3-3700 at 12.3 +- 1.8 x 10^-18 W m^-2. We use thermo-chemical disk models to model the gas emission, using constraints on the [OI] 63 micron, and ancillary data to derive gas mass upper limits and constrain gas-to-dust ratios. For HD 377 and HR 8799, we find 3 sigma upper limits on the gas mass of 0.1-20 Mearth. For RX J1852.3-3700, we find two distinct disk scenarios that could explain the detection of [OI] 63 micron and CO(2-1) upper limits reported from the literature: (i) a large disk with gas co-located with the dust (16-500 AU), resulting in a large tenuous disk with ~16 Mearth of gas, or (ii) an optically thick gas disk, truncated at ~70 AU, with a gas mass of 150 Mearth. We discuss the implications of these results for the formation and evolution of planets in these three systems.Comment: Accepted for publication in ApJ, 8 pages ApJ style (incl. references), 2 figures, 4 table