1,028 research outputs found
The Application of the Montage Image Mosaic Engine To The Visualization Of Astronomical Images
The Montage Image Mosaic Engine was designed as a scalable toolkit, written
in C for performance and portability across *nix platforms, that assembles FITS
images into mosaics. The code is freely available and has been widely used in
the astronomy and IT communities for research, product generation and for
developing next-generation cyber-infrastructure. Recently, it has begun to
finding applicability in the field of visualization. This has come about
because the toolkit design allows easy integration into scalable systems that
process data for subsequent visualization in a browser or client. And it
includes a visualization tool suitable for automation and for integration into
Python: mViewer creates, with a single command, complex multi-color images
overlaid with coordinate displays, labels, and observation footprints, and
includes an adaptive image histogram equalization method that preserves the
structure of a stretched image over its dynamic range. The Montage toolkit
contains functionality originally developed to support the creation and
management of mosaics but which also offers value to visualization: a
background rectification algorithm that reveals the faint structure in an
image; and tools for creating cutout and down-sampled versions of large images.
Version 5 of Montage offers support for visualizing data written in HEALPix
sky-tessellation scheme, and functionality for processing and organizing images
to comply with the TOAST sky-tessellation scheme required for consumption by
the World Wide Telescope (WWT). Four online tutorials enable readers to
reproduce and extend all the visualizations presented in this paper.Comment: 16 pages, 9 figures; accepted for publication in the PASP Special
Focus Issue: Techniques and Methods for Astrophysical Data Visualizatio
The Montage Image Mosaic Service: Custom Image Mosaics On-Demand
The Montage software suite has proven extremely useful as a general engine for reprojecting, background matching, and mosaicking astronomical image data from a wide variety of sources. The processing algorithms support all common World Coordinate System (WCS) projections and have been shown to be both astrometrically accurate and flux conserving. The background ‘matching’ algorithm does not remove background flux but rather finds the best compromise background based on all the input and matches the individual images to that. The Infrared Science Archive (IRSA), part of the Infrared Processing and Analysis Center (IPAC) at Caltech, has now wrapped the Montage software as a CGI service and provided a compute and request management infrastructure capable of producing approximately 2 TBytes / day of image mosaic output (e.g. from 2MASS and SDSS data). Besides the basic Montage engine, this service makes use of a 16-node LINUX cluster (dual processor, dual core) and the ROME request management software developed by the National Virtual Observatory (NVO). ROME uses EJB/database technology to manage user requests, queue processing and load balance between users, and managing job monitoring and user notification. The Montage service will be extended to process userdefined data collections, including private data uploads
A Cross-Match of 2MASS and SDSS: Newly-Found L and T Dwarfs and an Estimate of the Space Densitfy of T Dwarfs
We report new L and T dwarfs found in a cross-match of the SDSS Data Release
1 and 2MASS. Our simultaneous search of the two databases effectively allows us
to relax the criteria for object detection in either survey and to explore the
combined databases to a greater completeness level. We find two new T dwarfs in
addition to the 13 already known in the SDSS DR1 footprint. We also identify 22
new candidate and bona-fide L dwarfs, including a new young L2 dwarf and a
peculiar L2 dwarf with unusually blue near-IR colors: potentially the result of
mildly sub-solar metallicity. These discoveries underscore the utility of
simultaneous database cross-correlation in searching for rare objects. Our
cross-match completes the census of T dwarfs within the joint SDSS and 2MASS
flux limits to the 97% level. Hence, we are able to accurately infer the space
density of T dwarfs. We employ Monte Carlo tools to simulate the observed
population of SDSS DR1 T dwarfs with 2MASS counterparts and find that the space
density of T0-T8 dwarf systems is 0.0070 (-0.0030; +0.0032) per cubic parsec
(95% confidence interval), i.e., about one per 140 cubic parsecs. Compared to
predictions for the T dwarf space density that depend on various assumptions
for the sub-stellar mass function, this result is most consistent with models
that assume a flat sub-stellar mass function dN/dM ~ M^0. No >T8 dwarfs were
discovered in the present cross-match, though less than one was expected in the
limited area (2099 sq. degrees) of SDSS DR1.Comment: To appear in ApJ, Feb 10, 2008 issue. 37 pages, including 12 figures
and 14 table
Running a distributed virtual observatory: US Virtual Astronomical Observatory operations
Operation of the US Virtual Astronomical Observatory shares some issues with
modern physical observatories, e.g., intimidating data volumes and rapid
technological change, and must also address unique concerns like the lack of
direct control of the underlying and scattered data resources, and the
distributed nature of the observatory itself. In this paper we discuss how the
VAO has addressed these challenges to provide the astronomical community with a
coherent set of science-enabling tools and services. The distributed nature of
our virtual observatory-with data and personnel spanning geographic,
institutional and regime boundaries-is simultaneously a major operational
headache and the primary science motivation for the VAO. Most astronomy today
uses data from many resources. Facilitation of matching heterogeneous datasets
is a fundamental reason for the virtual observatory. Key aspects of our
approach include continuous monitoring and validation of VAO and VO services
and the datasets provided by the community, monitoring of user requests to
optimize access, caching for large datasets, and providing distributed storage
services that allow user to collect results near large data repositories. Some
elements are now fully implemented, while others are planned for subsequent
years. The distributed nature of the VAO requires careful attention to what can
be a straightforward operation at a conventional observatory, e.g., the
organization of the web site or the collection and combined analysis of logs.
Many of these strategies use and extend protocols developed by the
international virtual observatory community.Comment: 7 pages with 2 figures included within PD
A Cost-Benefit Study of Doing Astrophysics On The Cloud: Production of Image Mosaics
Utility grids such as the Amazon EC2 and Amazon S3 clouds offer computational and storage resources that can be used on-demand for a fee by compute- and data-intensive applications. The cost of running an application on such a cloud depends on the compute, storage and communication resources it will provision and consume. Different execution plans of the same application may result in significantly different costs. We studied via simulation the cost performance trade-offs of different execution and resource provisioning plans by creating, under the Amazon cloud fee structure, mosaics with the Montage image mosaic engine, a widely used data- and compute-intensive application. Specifically, we studied the cost of building mosaics of 2MASS data that have sizes of 1, 2 and 4 square degrees, and a 2MASS all-sky mosaic. These are examples of mosaics commonly generated by astronomers. We also study these trade-offs in the context of the storage and communication fees of Amazon S3 when used for long-term application data archiving. Our results show that by provisioning the right amount of storage and compute resources cost can be significantly reduced with no significant impact on application performance
Nitroheterocyclic drug resistance mechanisms in <i>Trypanosoma brucei</i>
OBJECTIVES: The objective of this study was to identify the mechanisms of resistance to nifurtimox and fexinidazole in African trypanosomes. METHODS: Bloodstream-form Trypanosoma brucei were selected for resistance to nifurtimox and fexinidazole by stepwise exposure to increasing drug concentrations. Clones were subjected to WGS to identify putative resistance genes. Transgenic parasites modulating expression of genes of interest were generated and drug susceptibility phenotypes determined. RESULTS: Nifurtimox-resistant (NfxR) and fexinidazole-resistant (FxR) parasites shared reciprocal cross-resistance suggestive of a common mechanism of action. Previously, a type I nitroreductase (NTR) has been implicated in nitro drug activation. WGS of resistant clones revealed that NfxR parasites had lost >100 kb from one copy of chromosome 7, rendering them hemizygous for NTR as well as over 30 other genes. FxR parasites retained both copies of NTR, but lost >70 kb downstream of one NTR allele, decreasing NTR transcription by half. A single knockout line of NTR displayed 1.6- and 1.9-fold resistance to nifurtimox and fexinidazole, respectively. Since NfxR and FxR parasites are ∼6- and 20-fold resistant to nifurtimox and fexinidazole, respectively, additional factors must be involved. Overexpression and knockout studies ruled out a role for a putative oxidoreductase (Tb927.7.7410) and a hypothetical gene (Tb927.1.1050), previously identified in a genome-scale RNAi screen. CONCLUSIONS: NTR was confirmed as a key resistance determinant, either by loss of one gene copy or loss of gene expression. Further work is required to identify which of the many dozens of SNPs identified in the drug-resistant cell lines contribute to the overall resistance phenotype
The organization and management of the Virtual Astronomical Observatory
The U.S. Virtual Astronomical Observatory (VAO; http://www.us-vao.org/) has
been in operation since May 2010. Its goal is to enable new science through
efficient integration of distributed multi-wavelength data. This paper
describes the management and organization of the VAO, and emphasizes the
techniques used to ensure efficiency in a distributed organization. Management
methods include using an annual program plan as the basis for establishing
contracts with member organizations, regular communication, and monitoring of
processes.Comment: 9 pages, 3 figures. SPIE Conference 8449: Modeling, Systems
Engineering, and Project Management for Astronomy
HST Fine Guidance Sensor Astrometric Parallaxes for Three Dwarf Novae: SS Aurigae, SS Cygni, and U Geminorum
We report astrometric parallaxes for three well known dwarf novae obtained
using the Fine Guidance Sensors on the Hubble Space Telescope. We found a
parallax for SS Aurigae of Pi = 5.00 +/- 0.64 mas, for SS Cygni we found Pi =
6.02 +/- 0.46 mas, and for U Geminorum we obtained Pi = 10.37 +/- 0.50 mas.
These represent the first true trigonometric parallaxes of any dwarf novae. We
briefly compare these results with previous distance estimates. This program
demonstrates that with a very modest amount of HST observing time, the Fine
Guidance Sensors can deliver parallaxes of unrivaled precision.Comment: 15 pages, 2 Table
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