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Game started three hours later once first of many patches downloaded. Two-hour break to recover from fainting when Star Wars logo and fanfare blare out from monitor. Wookiee character rolled up. Twenty minutes of messing around with the random name generator before finally settling on original choice of Flewbacca. Tutorial played. Another fainting break once Mos Eisley loads up. Several months of dedicated skill grinding coupled with a growing sense that this isn't actually the all-encompassing Star Wars online experience dreamt about. (For a start there's no space travel. Or lightsabers.) Continual depression at the lack of Star IVors-ness and the everdeepening grind. Unremitting joy half a year later at the release of the Jump To Lightspeed add-on, finally bringing space travel and combat to the universe.
One of the most intriguing results from HST has been the discovery of ultraluminous star clusters in interacting and merging galaxies. These clusters have the luminosities, colors, and sizes that would be expected of young globular clusters produced by the interaction. We propose to use the data in the HST Archive to determine how prevalent this phenomena is, and to determine whether similar clusters are produced in other environments. Three samples will be extracted and studied in a systematic and consistent manner: 1} interacting and merging galaxies, 2} starburst galaxies, 3} a control sample of ``normal'' galaxies. A preliminary search of the archives shows that there are at least 20 galaxies in each of these samples, and the number will grow by about 50 observations become available. The data will be used to determine the luminosity function, color histogram , spatial distribution, and structural properties of the clusters using the same techniques employed in our study of NGC 7252 ``Atoms -for-Peace'' galaxy and NGC 4038/4039 ``The Antennae''. Our ultimate goals are: 1} to understand how globular clusters form, and 2} to use the clusters as evolutionary tracers to unravel the histories of interacting galaxies.
Astronomical instruments produce petabytes of images every year, vastly more than can be inspected by a member of the astronomical community in search of a specific population of structures. Fortunately, the sky is mostly black and source extraction algorithms have been developed to provide searchable catalogs of unconfused sources like stars and galaxies. These tools often fail for studies of more diffuse structures like the interstellar medium and unresolved stellar structures in nearby galaxies, leaving astronomers interested in observations of photodissociation regions, stellar clusters, diffuse interstellar clouds without the crucial ability to search. In this work we present a new path forward for finding structures in large data sets similar to an input structure using convolutional neural networks, transfer learning, and machine learning clustering techniques. We show applications to archival data in the Mikulski Archive for Space Telescopes (MAST).
With no future space ultraviolet instruments currently planned, the data from the UV spectrographs aboard the Hubble Space Telescope have a legacy value beyond their initial science goals. The Hubble Spectroscopic Legacy Archive will provide to the community new science-grade combined spectra for all publicly available data obtained by the Cosmic Origins Spectrograph (COS) and the Space Telescope Imaging Spectrograph (STIS). These data will be packaged into "smart archives" according to target type and scientific themes to facilitate the construction of archival samples for common science uses. A new "quick look" capability will make the data easy for users to quickly access, assess the quality of, and download for archival science starting in Cycle 24, with the first generation of these products for the FUV modes of COS available online via MAST in early 2016.
Observations of the Universe on scales smaller than typical, massive galaxies challenge the standard Lambda Cold Dark Matter paradigm for structure formation. It is thus imperative to discover and characterize the faintest dwarf galaxy systems, not just within the Local Group, but in relatively isolated environments as well in order to properly connect them with models of structure formation. Here we report on a systematic search of public ultraviolet and optical archives for dwarf galaxy counterparts to so-called Ultra Compact High Velocity Clouds (UCHVCs), which are compact, isolated HI sources recently found in the Galactic Arecibo L-band Feed Array-HI (GALFA-HI) and Arecibo Legacy Fast ALFA (ALFALFA-HI) surveys. Our search has uncovered at least three strong dwarf galaxy candidates, and we present their inferred star formation rate and structural properties here.
WFIRST's unique combination of a large (0.3 deg2) field of view and HST-like angular resolution and sensitivity in the near infrared will produce spectacular new insights into the origins of stars, galaxies, and structure in the cosmos. We propose a WFIRST Archive Science Investigation Team (SIT-F) to define an archival, query, and analysis system that will enable scientific discovery in all relevant areas of astrophysics and maximize the overall scientific yield of the mission. Guest investigators (GIs), guest observers (GOs), the WFIRST SIT's, WFIRST Science Center(s), and astronomers using data from other surveys will all benefit from the extensive, easy, fast and reliable use of the WFIRST archives. We propose to develop the science requirements for the archive and work to understand its interactions with other elements of the WFIRST mission. To accomplish this, we will conduct case studies to derive performance requirements for the WFIRST archives. These will clarify what is needed for GIs to make important scientific discoveries across a broad range of astrophysics. While other SITs will primarily address the science capabilities of the WFIRST instruments, we will look ahead to the science enabling capabilities of the WFIRST archives. We will demonstrate how the archive can be optimized to take advantage of the extraordinary science capabilities of the WFIRST instruments as well as major space and ground observatories to maximize the science return of the mission. We will use the "20 queries" methodology, formulated by Jim Gray, to cover the most important science analysis patterns and use these to establish the performance required of the WFIRST archive. The case studies will be centered on studying galaxy evolution as a function of cosmic time, environment and intrinsic properties. The analyses will require massive angular and spatial cross correlations between key galaxy properties to search for new fundamental scaling relations that may only become
Historically, astronomers have utilized a piecemeal set of archives such as SIMBAD, the Washington Double Star Catalog, various exoplanet encyclopedias and electronic tables from the literature to cobble together stellar and exo-planetary parameters in the absence of corresponding images and spectra. As the search for planets around young stars through direct imaging, transits and infrared/optical radial velocity surveys blossoms, there is a void in the available set of to create comprehensive lists of the stellar parameters of nearby stars especially for important parameters such as metallicity and stellar activity indicators. For direct imaging surveys, we need better resources for downloading existing high contrast images to help confirm new discoveries and find ideal target stars. Once we have discovered new planets, we need a uniform database of stellar and planetary parameters from which to look for correlations to better understand the formation and evolution of these systems. As a solution to these issues, we are developing the Starchive - an open access stellar archive in the spirit of the open exoplanet catalog, the Kepler Community Follow-up Program and many others. The archive will allow users to download various datasets, upload new images, spectra and metadata and will contain multiple plotting tools to use in presentations and data interpretations. While we will highly regulate and constantly validate the data being placed into our archive the open nature of its design is intended to allow the database to be expanded efficiently and have a level of versatility which is necessary in today's fast moving, big data community. Finally, the front-end scripts will be placed on github and users will be encouraged to contribute new plotting tools. Here, I will introduce the community to the content and expected capabilities of the archive and query the audience for community feedback. 2ff7e9595c
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