[ { "id": "authors:p828p-sky71", "collection": "authors", "collection_id": "p828p-sky71", "cite_using_url": "https://resolver.caltech.edu/CaltechCACR:2004.218", "type": "conference_item", "title": "Palomar-QUEST: A case study in designing sky surveys in the VO era", "author": [ { "family_name": "Graham", "given_name": "Matthew J.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Williams", "given_name": "Roy", "clpid": "Williams-R" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Mahabal", "given_name": "Ashish", "orcid": "0000-0003-2242-0244", "clpid": "Mahabal-A-A" }, { "family_name": "Baltay", "given_name": "Charles", "clpid": "Baltay-C" }, { "family_name": "Rabinowitz", "given_name": "Dave", "clpid": "Rabinowitz-D" }, { "family_name": "Bauer", "given_name": "Anne", "clpid": "Bauer-A" }, { "family_name": "Snyder", "given_name": "Jeff", "clpid": "Snyder-J" }, { "family_name": "Morgan", "given_name": "Nick", "clpid": "Morgan-N" }, { "family_name": "Andrews", "given_name": "Peter", "clpid": "Andrews-P" }, { "family_name": "Szalay", "given_name": "Alexander S.", "clpid": "Szalay-A-S" }, { "family_name": "Brunner", "given_name": "Robert J.", "clpid": "Brunner-R-J" }, { "family_name": "Musser", "given_name": "Jim", "clpid": "Musser-J" } ], "abstract": "The advent of wide-area multicolour synoptic sky surveys is\nleading to data sets unprecedented in size, complexity and data through-\nput. VO technology offers a way to exploit these to the full but re-\nquires changes in design philosophy. The Palomar-QUEST survey is a\nmajor new survey being undertaken by Caltech, Yale, JPL and Indi-\nana University to repeatedly observe\n1/3 of the sky (\u223c 15000 sq. deg. between \u201327\u00b0 \u2264\n \u03b4 \u2264 27\u00b0) in seven passbands. Utilising the 48-inch\nOschin Schmidt Telescope at the Palomar Observatory with the 112-CCD\nQUEST camera covering the full 4\u00b0 x 4\u00b0 field of view, it will generate\n\u223c 1TB of data per month. In this paper, we review the design of QUEST\nas a VO resource, a federated data set and an exemplar of VO standards.", "publisher": "Caltech Library", "publication_date": "2004-10" }, { "id": "authors:thwec-a0060", "collection": "authors", "collection_id": "thwec-a0060", "cite_using_url": "https://resolver.caltech.edu/CaltechCACR:2004.219", "type": "conference_item", "title": "Exploring the Time Domain with the Palomar-QUEST Sky Survey", "author": [ { "family_name": "Mahabal", "given_name": "A.", "orcid": "0000-0003-2242-0244", "clpid": "Mahabal-A-A" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Graham", "given_name": "M.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Williams", "given_name": "R.", "clpid": "Williams-R" }, { "family_name": "Granett", "given_name": "B.", "clpid": "Granett-B" }, { "family_name": "Bogosavljevic", "given_name": "M.", "clpid": "Bogosavljevic-M" }, { "family_name": "Baltay", "given_name": "C.", "clpid": "Baltay-C" }, { "family_name": "Rabinowitz", "given_name": "D.", "clpid": "Rabinowitz-D" }, { "family_name": "Bauer", "given_name": "A.", "clpid": "Bauer-A" }, { "family_name": "Andrews", "given_name": "P.", "clpid": "Andrews-P" }, { "family_name": "Morgan", "given_name": "N.", "clpid": "Morgan-N" }, { "family_name": "Snyder", "given_name": "J.", "clpid": "Snyder-J" }, { "family_name": "Ellman", "given_name": "N.", "clpid": "Ellman-N" }, { "family_name": "Duffau", "given_name": "S.", "clpid": "Duffau-S" }, { "family_name": "Musser", "given_name": "J.", "clpid": "Musser-J" }, { "family_name": "Mufson", "given_name": "S.", "clpid": "Mufson-S" }, { "family_name": "Gebhard", "given_name": "M.", "clpid": "Gebhard-M" }, { "family_name": "Brunner", "given_name": "R.", "clpid": "Brunner-R" }, { "family_name": "Rengstorf", "given_name": "A.", "clpid": "Rengstorf-A" } ], "abstract": "Discoveries in astronomy are often made through a systematic exploration of\npreviously poorly covered regions of the observable parameter space [1,2]. In\nparticular, exploration of the time variability on the sky over a broad range of\nux levels and wavelengths is rapidly becoming a new frontier of astronomical\nresearch [3,4]. Many exciting astrophysical phenomena are known in the time\ndomain: all manner of variable stars, stellar explosions such as SNe and GRBs,\nvariable AGN, pulsars, microlensing events, etc. Yet undoubtedly many more\nremain to be discovered.\nA number of surveys and experiments exploring the time domain are already\nin progress (see, e.g., [5,6] for listings), and even more ambitious synoptic sky\nsurveys are being planned, e.g., [7,8]. The important factors in such programs\nare (1) the area covered, (2) the depth of coverage, (3) number of wavelengths\nused, and (4) the baseline(s) in time.", "publisher": "Caltech Library", "publication_date": "2004-10" }, { "id": "authors:10mfc-rds74", "collection": "authors", "collection_id": "10mfc-rds74", "cite_using_url": "https://resolver.caltech.edu/CaltechCACR:2003.202", "type": "conference_item", "title": "Hyperatlas: A New Framework for Image Federation", "author": [ { "family_name": "Williams", "given_name": "R. D.", "orcid": "0000-0002-9145-8580", "clpid": "Williams-R-D" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Feldmann", "given_name": "M. T.", "clpid": "Feldmann-M-T" }, { "family_name": "Jacob", "given_name": "J. C.", "clpid": "Jacob-J-C" } ], "abstract": "Hyperatlas is an open standard intended to facilitate the large-scale federation of image-based data. The subject of hyperatlas is the space of sphere-to-plane projection mappings (the FITS-WCS information), and the standard consists of coherent collections of these on which data can be resampled and thereby federated with other image data. We hope for a distributed effort that will produce a multi-faceted image atlas of the sky, made by federating many different surveys at different wavelengths and different times. We expect that hyperatlas-compliant imagery will be published and discovered through an International Virtual Observatory Alliance (IVOA) registry, and that grid-based services will emerge for the required resampling and mosaicking.", "doi": "10.48550/arXiv.0312195", "publication_date": "2003" }, { "id": "authors:jye65-rg886", "collection": "authors", "collection_id": "jye65-rg886", "cite_using_url": "https://resolver.caltech.edu/CaltechCACR:2002.003", "type": "conference_item", "title": "Atlasmaker: A Grid-based Implementation of the Hyperatlas", "author": [ { "family_name": "Williams", "given_name": "R. D.", "orcid": "0000-0002-9145-8580", "clpid": "Williams-R-D" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Feldmann", "given_name": "M. T.", "clpid": "Feldmann-M-T" }, { "family_name": "Jacob", "given_name": "J. C.", "clpid": "Jacob-J-C" } ], "abstract": "The Atlasmaker project is using Grid technology, in combination with NVO interoperability, to create new knowledge resources in astronomy. The product is a multi-faceted, multi-dimensional, scientifically trusted image atlas of the sky, made by federating many different surveys at different wavelengths, times, resolutions, polarizations, etc. The Atlasmaker software does resampling and mosaicking of image collections, and is well-suited to operate with the Hyperatlas standard. Requests can be satisfied via on-demand computations or by accessing a data cache. Computed data is stored in a distributed virtual file system, such as the Storage Resource Broker (SRB). We expect these atlases to be a new and powerful paradigm for knowledge extraction in astronomy, as well as a magnificent way to build educational resources. The system is being incorporated into the data analysis pipeline of the Palomar-Quest synoptic survey, and is being used to generate all-sky atlases from the 2MASS, SDSS, and DPOSS surveys for joint object detection.", "doi": "10.48550/arXiv.0312196", "publication_date": "2002" }, { "id": "authors:8z0g2-ymt52", "collection": "authors", "collection_id": "8z0g2-ymt52", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190807-085154076", "type": "conference_item", "title": "A rich nearby cluster in Sagittarius", "author": [ { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "de Carvalho", "given_name": "R. R.", "orcid": "0000-0002-1283-3363", "clpid": "de-Carvalho-R-R" }, { "family_name": "Thompson", "given_name": "D. J.", "clpid": "Thompson-D-J" }, { "family_name": "Mould", "given_name": "J. R.", "orcid": "0000-0003-3820-1740", "clpid": "Mould-J-R" } ], "abstract": "In a series of ESO Messenger and Comptes Rendu papers (1978 - 1985), Terzan, Bernard, and Ju discovered some 45 diffuse objects in the general direction of the Galactic Bulge, viz., Sagittarius bright cloud B, \u03b1 range 17^h04^m \u2013 17^h42^m, \u03b4 range -24\u00b0 to -33\u00b0. This region, centered near 1_(II) ~358\u00b0, b_(II) ~ +7\u00b0, has a patchy, but obviously very heavy extinction (we estimate A_v > 3^m \u2013 4^m). These TBJ objects are a mixed bag; in the discovery papers, some were tentatively classified as galaxies, some as possible globular clusters, others as planetary nebulae. During an imaging search for obscured globular clusters, one of us (SGD) obtained images of 14 of them. Out of those, two turned out to be probable globular clusters (TJ 5 and TJ 23), one planetary nebula. (TBJ 41), and the rest were obviously galaxies. A dozen of the remaining objects may be classified as galaxies from their appearance on the SRC/I sky survey films. The magnitudes of detected galaxies are typically in the range R ~17^m \u2013 18^m, within 10 - 20 arcsec apertures (the measurements are difficult and still very preliminary, because of the heavy stellar foreground). The occurrence of so many background galaxies in a. relatively small and heavily obscured area is remarkable. These objects must be luminous ellipticals and/or bright S0 or Sp bulges: anything with a lower surface brightness would not be detected through the heavy extinction and foreground. (None of the TBJ galaxies and possible galaxies a.re detected in the IRAS PSC, which corroborates their identification as early types.) Thus, this concentration of galaxies must be just the very tip of an iceberg. Terzan et al. apparently discovered a major rich cluster, hidden behind the Galactic Bulge, in the heart of \"zone of avoidance\".", "publisher": "Caltech Library", "publication_date": "1989-05" }, { "id": "authors:d5zmv-mag75", "collection": "authors", "collection_id": "d5zmv-mag75", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190807-083113838", "type": "conference_item", "title": "A photometric distance-indicator relation for low surface brightness dwarfs", "author": [ { "family_name": "de Carvalho", "given_name": "R. R.", "orcid": "0000-0002-1283-3363", "clpid": "de-Carvalho-R-R" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" } ], "abstract": "Recently, dwarf elliptical galaxies have received a great deal of attention and some of the points to be addressed in future investigations include metallicities of the stellar population, structural properties, and the large scale distribution (Caldwell and Bothun 1987; Impey et al. 1988; Eder et al. 1989). Here we are more concerned with the large scale structure for this class of galaxies. Recent analysis by Eder et al. (1989) has indicated that dwarf galaxies seem to trace the large scale structures in the same way as bright ones. Another important characteristic of dwarfs is that they are more populous in clusters than bright elliptical galaxies. The ratio dE/E (dwarf/normal) in Fomax is around 4, and in Virgo 17, which means that if we can define a distance indicator relation for dwarfs with at least the same accuracy as we have for normal ellipticals, we can substantially improve our distance measurement for clusters, thus mapping the large-scale velocity field more efficiently.", "publisher": "Caltech Library", "publication_date": "1989-05" } ]