[ { "id": "authors:xdcnw-40p66", "collection": "authors", "collection_id": "xdcnw-40p66", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190107-144131759", "type": "book_section", "title": "Prime Focus Spectrograph (PFS) for the Subaru telescope: ongoing integration and future plans", "book_title": "Ground-based and Airborne Instrumentation for Astronomy VII", "author": [ { "family_name": "Tamura", "given_name": "Naoyuki", "clpid": "Tamura-Naoyuki" }, { "family_name": "Burnham", "given_name": "Jill A.", "clpid": "Burnham-J-A" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Dekany", "given_name": "Richard G.", "clpid": "Dekany-Richard" }, { "family_name": "Hover", "given_name": "David J.", "clpid": "Hover-D-J" }, { "family_name": "Reiley", "given_name": "Daniel J.", "clpid": "Reiley-D-J" }, { "family_name": "Roberts", "given_name": "Mitsuko", "clpid": "Roberts-Mitsuko" } ], "contributor": [ { "family_name": "Evans", "given_name": "Christopher J.", "clpid": "Evans-C-J" }, { "family_name": "Simard", "given_name": "Luc", "clpid": "Simard-L" }, { "family_name": "Takami", "given_name": "Hideki", "clpid": "Takami-Hideki" } ], "abstract": "PFS (Prime Focus Spectrograph), a next generation facility instrument on the 8.2-meter Subaru Telescope, is a very wide-field, massively multiplexed, optical and near-infrared spectrograph. Exploiting the Subaru prime focus, 2394 reconfigurable fibers will be distributed over the 1.3 deg field of view. The spectrograph has been designed with 3 arms of blue, red, and near-infrared cameras to simultaneously observe spectra from 380nm to 1260nm in one exposure at a resolution of ~ 1.6-2.7\u00c5. An international collaboration is developing this instrument under the initiative of Kavli IPMU. The project recently started undertaking the commissioning process of a subsystem at the Subaru Telescope side, with the integration and test processes of the other subsystems ongoing in parallel. We are aiming to start engineering night-sky operations in 2019, and observations for scientific use in 2021. This article gives an overview of the instrument, current project status and future paths forward.", "doi": "10.1117/12.2311871", "isbn": "9781510619579", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-27", "pages": "Art. No. 107021C" }, { "id": "authors:febay-0cf98", "collection": "authors", "collection_id": "febay-0cf98", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170217-081936401", "type": "book_section", "title": "Prime Focus Spectrograph (PFS) for the Subaru Telescope: Overview, recent progress, and future perspectives", "book_title": "Ground-based and Airborne Instrumentation for Astronomy VI", "author": [ { "family_name": "Tamura", "given_name": "Naoyuki", "clpid": "Tamura-Naoyuki" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Dekany", "given_name": "Richard G.", "clpid": "Dekany-Richard" }, { "family_name": "Mao", "given_name": "Peter", "clpid": "Mao-Peter" }, { "family_name": "Reiley", "given_name": "Daniel J.", "clpid": "Reiley-D-J" }, { "family_name": "Roberts", "given_name": "Mitsuko", "clpid": "Roberts-Mitsuko" } ], "contributor": [ { "family_name": "Evans", "given_name": "Christopher J.", "clpid": "Evans-C-J" }, { "family_name": "Simard", "given_name": "Luc", "clpid": "Simard-L" }, { "family_name": "Takami", "given_name": "Hideki", "clpid": "Takami-Hideki" } ], "abstract": "PFS (Prime Focus Spectrograph), a next generation facility instrument on the 8.2-meter Subaru Telescope, is a very wide-field, massively multiplexed, optical and near-infrared spectrograph. Exploiting the Subaru prime focus, 2394 reconfigurable fibers will be distributed over the 1.3 deg field of view. The spectrograph has been designed with 3 arms of blue, red, and near-infrared cameras to simultaneously observe spectra from 380nm to 1260nm in one exposure at a resolution of ~1.6-2.7\u00c5. An international collaboration is developing this instrument under the initiative of Kavli IPMU. The project is now going into the construction phase aiming at undertaking system integration in 2017-2018 and subsequently carrying out engineering operations in 2018-2019. This article gives an overview of the instrument, current project status and future paths forward.", "doi": "10.1117/12.2232103", "isbn": "978-1-5106-0196-3", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2016-08-09", "pages": "Art. No. 99081M" }, { "id": "authors:dxx0h-hs287", "collection": "authors", "collection_id": "dxx0h-hs287", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160208-140133188", "type": "book_section", "title": "The Outer Galactic Halo As Probed By RR Lyr Stars From the Palomar Transient Facility + Keck", "book_title": "The General Assembly of Galaxy Halos: Structure, Origin and Evolution", "author": [ { "family_name": "Cohen", "given_name": "Judith", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Sesar", "given_name": "Branimir", "orcid": "0000-0002-0834-3978", "clpid": "Sesar-B" }, { "family_name": "Banholzer", "given_name": "Sophianna", "clpid": "Banholzer-S" }, { "literal": "PTF Collaboration" } ], "contributor": [ { "family_name": "Bragaglia", "given_name": "Angela", "clpid": "Bragaglia-A" }, { "family_name": "Arnaboldi", "given_name": "Magda", "clpid": "Arnaboldi-M" }, { "family_name": "Rejkuba", "given_name": "Marina", "clpid": "Rejkuba-M" }, { "family_name": "Romano", "given_name": "Donatella", "clpid": "Romano-D" } ], "abstract": "We present initial results from our study of the outer halo of the Milky Way using a large sample of RR Lyr(ab) variables datamined from the archives of the Palomar Transient Facility. Of the 464 RR Lyr in our sample with distances exceeding 50 kpc, 62 have been observed spectroscopically at the Keck Observatory. v _r and \u03c3(v_r) are given as a function of distance between 50 and 110 kpc, and a very preliminary rather low total mass for the Milky Way out to 110 kpc of ~7 \u00b1 1.5 \u00d7 10^(11) M\u2299 is derived from our data.", "doi": "10.1017/S174392131500976X", "isbn": "9781107138193", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2016-05-09", "pages": "91-96" }, { "id": "authors:16gdh-wz856", "collection": "authors", "collection_id": "16gdh-wz856", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121022-131934431", "type": "book_section", "title": "Outliers in the 0Z Survey", "book_title": "Galactic Archaeology: Near-Field Cosmology and the Formation of the Milky Way", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Christlieb", "given_name": "Norbert", "orcid": "0000-0002-4043-2727", "clpid": "Christlieb-N" }, { "family_name": "Thompson", "given_name": "Ian", "clpid": "Thompson-I" }, { "family_name": "McWilliam", "given_name": "Andrew", "clpid": "McWilliam-A" }, { "family_name": "Shectman", "given_name": "Stephen", "clpid": "Shectman-S" } ], "contributor": [ { "family_name": "Aoki", "given_name": "Wako", "clpid": "Aoki-Wako" }, { "family_name": "Ishigaki", "given_name": "M.", "clpid": "Ishigaki-M" }, { "family_name": "Suda", "given_name": "T.", "clpid": "Suda-T" }, { "family_name": "Tsujimoto", "given_name": "T.", "clpid": "Tsujimoto-T" }, { "family_name": "Arimoto", "given_name": "N.", "clpid": "Arimoto-Nobuo" } ], "abstract": "We have now completed detailed abundance analyses of more than 100 stars selected as candidate extremely metal-poor stars with [Fe/H] < \u20133.0 dex. Of these 18 are below \u20133.3 dex on the scale of the First Stars VLT project led by Cayrel, and 57 are below \u20133.0 dex on that scale. Ignoring enhancement of carbon which ranges up to very large values, and two C-rich stars with very high N as well, there are 0 to 3 high or low strong outliers for each abundance ratio tested from Mg to Ni. The outliers have been checked and they are real. Ignoring the outliers, the dispersions are in most cases approximately consistent with the uncertainties, except those for [Sr/Fe] and [Ba/Fe], which are much larger. Approximately 6% of the sample are strong outliers in one or more elements between Mg and Ni. This rises to \u223c15% if minor outliers for these elements and strong outliers for Sr and Ba are included. There are 6 stars with extremely low [Sr/Fe] and [Ba/Fe], including one which has lower [Ba/H] than Draco 119, the star found by Fulbright, Rich & Castro to have the lowest such ratio known previously. There is one extreme r-process star.", "doi": "10.48550/arXiv.1201.4190", "isbn": "978-1-58381-798-8", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2012-08-25", "pages": "61-64" }, { "id": "authors:6wp3q-09890", "collection": "authors", "collection_id": "6wp3q-09890", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121022-131846051", "type": "book_section", "title": "The Chemical Evolution of Milky Way Satellite Galaxies from Keck/DEIMOS Multi-Element Abundance Measurements", "book_title": "Galactic Archaeology: Near-Field Cosmology and the Formation of the Milky Way", "author": [ { "family_name": "Kirby", "given_name": "Evan N.", "orcid": "0000-0001-6196-5162", "clpid": "Kirby-E-N" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Aoki", "given_name": "W.", "clpid": "Aoki-W" }, { "family_name": "Ishigaki", "given_name": "M.", "clpid": "Ishigaki-M" }, { "family_name": "Suda", "given_name": "T.", "clpid": "Suda-T" }, { "family_name": "Tsujimoto", "given_name": "T.", "clpid": "Tsujimoto-T" }, { "family_name": "Arimoto", "given_name": "N.", "clpid": "Arimoto-N" } ], "abstract": "A Keck/DEIMOS spectroscopic campaign of eight Milky Way (MW)\ndwarf spheroidal (dSph) satellite galaxies has generated spectral synthesis-based abundance measurements for nearly 3000 stars. The elements measured are Fe and the elements Mg, Si, Ca, and Ti. The dSph metallicity distributions show that the histories of the less luminous dSphs were marked by massive amounts of gas loss. The [/Fe] distributions indicate that the early star formation histories of most dSphs were very similar and that Type Ia supernova ejecta contributed to the abundances of all but the most metal-poor ([Fe/H] < \u22122.5) stars.", "isbn": "978-1-58381-798-8", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2012-08-25", "pages": "329-330" }, { "id": "authors:xmkhh-mp657", "collection": "authors", "collection_id": "xmkhh-mp657", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101101-112231015", "type": "book_section", "title": "Globular cluster abundances and what they can tell us about galaxy formation", "book_title": "Star clusters: basic galactic building blocks throughout time and space", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "DeGrijs", "given_name": "R.", "clpid": "DeGrijs-R" }, { "family_name": "Lepine", "given_name": "J. R. D.", "clpid": "Lepine-J-R-D" } ], "abstract": "We review the properties of globular clusters (GCs) which make them useful for studying the Galactic halo, Galactic chemical evolution and the early stages of the formation of the Milky Way. We review the evidence that GCs have a chemical inventory similar to those of halo field stars. We discuss the abundance ratios for dSph galaxies and show that it is possible to have formed at least part of the Galactic-halo field stellar population by dissolving GCs and/or accreting dSph galaxies, but only if this occurred at an early stage in the formation of the Galaxy. We review the constraints on halo-formation timescales deduced from the low magnesium isotopic ratios in metal-poor halo field dwarfs, which indicate that asymptotic giant-branch (AGB) stars did not have time to contribute significantly, while M71 contains two populations, one without and also one with a substantial AGB contribution. We review the limited evidence for GCs with a second population showing additional contributions from Type II supernovae, currently confined to \u03c9 Cen, M54 and M22, all of which may have been the nuclei or central regions of accreted galaxies. We check our own data for additional similar GCs and find preliminary indications that NGC 2419, a massive GC far in the outer Galactic halo, may also belong to this group.", "doi": "10.1017/S1743921309990998", "isbn": "9780-521-76484-1", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2009-08", "pages": "149-156" }, { "id": "authors:e553m-qkm70", "collection": "authors", "collection_id": "e553m-qkm70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100511-100205127", "type": "book_section", "title": "IR Integrated Light Colors For Galactic GCs and An Update on Young M31 Globular Clusters", "book_title": "Globular Clusters - Guides to Galaxies", "author": [ { "family_name": "Cohen", "given_name": "Judith", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Richtler", "given_name": "Tom", "clpid": "Richtler-T" }, { "family_name": "Larsen", "given_name": "S\u00f8ren", "clpid": "Larsen-S-S" } ], "abstract": "In our recent publication, Cohen, Matthews and Cameron [3], we presented observations made with the newly commissioned Keck laser-guide star adaptive optics system of 6 objects in M31 that are alleged in multiple recent studies to be young globular clusters (GCs); all are supposed to have ages\n\u22645 Gyr. The resulting FWHM of the PSF core in our images was ~70 mas. The four youngest of these objects are asterisms; they are with certainty not young GCs in M31. Based on their morphology, the two oldest are GCs in\nM31. While the M31 GCs with ages 5\u20138 Gyr appear to be mostly genuine, it appears that many of the alleged very young GCs in M31 are spurious identifications. This problem will be even more severe in studies of the GC systems of more distant spiral galaxies now underway, for which imaging at the spatial resolution of our observations in M31 may not be adequate to detect sample contamination by asterisms.\nHere we provide a brief update for this work.", "doi": "10.1007/978-3-540-76961-3_45", "isbn": "978-3-540-76960-6", "publisher": "Springer", "place_of_publication": "New York, NY", "publication_date": "2009", "pages": "189-192" }, { "id": "authors:e7qrb-6qn28", "collection": "authors", "collection_id": "e7qrb-6qn28", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122926622", "type": "book_section", "title": "Abundances in Galactic Bulge Dwarfs and the Origin of the Elements in the Bulge", "author": [ { "family_name": "Johnson", "given_name": "Jeniffer A.", "orcid": "0000-0001-9808-7172", "clpid": "Johnson-J-A" }, { "family_name": "Gould", "given_name": "Andrew", "clpid": "Gould-A-P" }, { "family_name": "Gaudi", "given_name": "B. Scott", "orcid": "0000-0003-0395-9869", "clpid": "Gaudi-B-S" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Huang", "given_name": "Wenjin", "clpid": "Huang-Wenjin" }, { "family_name": "Gal-Yam", "given_name": "Avishay", "orcid": "0000-0002-3653-5598", "clpid": "Gal-Yam-A" }, { "family_name": "Leonard", "given_name": "Douglas C.", "clpid": "Leonard-D-C" }, { "family_name": "Simon", "given_name": "Joshua D.", "clpid": "Simon-J-D" }, { "family_name": "Udalski", "given_name": "Andrzej", "orcid": "0000-0001-5207-5619", "clpid": "Udalski-A" }, { "family_name": "Bond", "given_name": "Ian A.", "clpid": "Bond-I-A" }, { "family_name": "Sumi", "given_name": "Takahiro", "clpid": "Sumi-Takahiro" } ], "abstract": "The Galactic Bulge has a very different chemical evolution history than the Milky Way disk or halo. The unique mix of supernovae and asymptotic giant branch stars that have contributed to the elements in the bulge offer the opportunity to identify or confirm the nucleosynthesis sites of elements. Abundance measurements based on the spectra of Galactic bulge dwarfs provide the only reliable measurements of the evolution of C and N in the Bulge, and have also been the source of the first measurements of S, K, Zn, Cu and Ba. We report on the use of gravitational microlensing to observe very faint Galactic bulge dwarfs and discuss the implications of these measurements for the origin of the elements. In particular, we argue that Type Ia SNe are unlikely to be important sources of Zn, but while the data on C and N suggest that asymptotic giant stars contributed to the chemical enrichment of the bulge, the data on Ba suggest that there was a delay before substantial AGB star production.", "doi": "10.22323/1.053.0024", "publisher": "SISSA", "publication_date": "2008-08" }, { "id": "authors:tbbfk-m5461", "collection": "authors", "collection_id": "tbbfk-m5461", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190516-142246247", "type": "book_section", "title": "MAGIQ at the W. M. Keck Observatory: initial deployment of a new acquisition, guiding, and image quality monitoring system", "book_title": "Ground-based and Airborne Instrumentation for Astronomy II", "author": [ { "family_name": "Adkins", "given_name": "Sean M.", "clpid": "Adkins-S-M" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Aycock", "given_name": "Joel", "clpid": "Aycock-J" }, { "family_name": "Bell", "given_name": "James", "orcid": "0000-0002-2006-4074", "clpid": "Bell-J-F-III" }, { "family_name": "Cohen", "given_name": "Richard", "clpid": "Cohen-R-W" }, { "family_name": "Cooper", "given_name": "Andrew", "clpid": "Cooper-A-P" }, { "family_name": "Goodrich", "given_name": "Bob", "clpid": "Goodrich-B" }, { "family_name": "Johnson", "given_name": "Jimmy", "clpid": "Johnson-J" }, { "family_name": "Kwok", "given_name": "Shui H.", "clpid": "Kwok-Shui-H" }, { "family_name": "Lyke", "given_name": "Jim", "clpid": "Lyke-J" }, { "family_name": "McCann", "given_name": "Kevin", "clpid": "McCann-K" }, { "family_name": "Neyman", "given_name": "Chris", "clpid": "Neyman-C-R" }, { "family_name": "Nordin", "given_name": "Tom", "clpid": "Nordin-T" }, { "family_name": "Panteleev", "given_name": "Sergey", "clpid": "Panteleev-S" }, { "family_name": "Tolleth", "given_name": "Grant", "clpid": "Tolleth-G" }, { "family_name": "Tsubota", "given_name": "Myrna", "clpid": "Tsubota-Myrna" } ], "contributor": [ { "family_name": "McLean", "given_name": "Ian S.", "clpid": "McLean-I-S" }, { "family_name": "Casali", "given_name": "Mark M.", "clpid": "Casali-M-M" } ], "abstract": "The W. M. Keck Observatory has completed the development and initial deployment of MAGIQ, the Multi-function Acquisition, Guiding and Image Quality monitoring system. MAGIQ is an integrated system for acquisition, guiding and image quality measurement for the Keck telescopes. This system replaces the acquisition and guiding hardware and software for existing instruments at the Observatory and is now the standard for visible wavelength band acquisition cameras for future instrumentation. In this paper we report on the final design and implementation of this new system, which includes three major components: a visible wavelength band acquisition camera, image quality measurement capability, and software for acquisition, guiding and image quality monitoring. The overall performance is described, as well as the details of our approach to integrating low order wavefront sensing capability in order to provide closed loop control of telescope focus.", "doi": "10.1117/12.789857", "isbn": "9780819472243", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2008-07-09", "pages": "Art. No. 70141U" }, { "id": "authors:tfaj1-q4x11", "collection": "authors", "collection_id": "tfaj1-q4x11", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100707-132658295", "type": "book_section", "title": "An Update on the 0Z Project", "book_title": "First stars III : Santa Fe, New Mexico, 15-20 July 2007", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Christlieb", "given_name": "N.", "orcid": "0000-0002-4043-2727", "clpid": "Christlieb-N" }, { "family_name": "McWilliam", "given_name": "A.", "clpid": "McWilliam-A" }, { "family_name": "Shectman", "given_name": "S.", "clpid": "Shectman-S" }, { "family_name": "Thompson", "given_name": "I.", "clpid": "Thompson-I" } ], "abstract": "We give an update on our 0Z Survey to find more extremely metal poor (EMP) stars with [Fe/H]<\u22123 dex through mining the database of the Hamburg/ESO Survey. We present the most extreme such stars we have found from ~1550 moderate resolution follow up spectra. One of these, HE1424\u20130241, has highly anomalous abundance ratios not seen in any previously known halo giant, with very deficient Si, moderately deficient Ca and Ti, highly enhanced Mn and Co, and low C, all with respect to Fe. We suggest a SNII where the nucleosynthetic yield for explosive \u03b1\u2013burning nuclei was very low compared to that for the hydrostatic \u03b1\u2013burning element Mg, which is normal in this star relative to Fe. A second, less extreme, outlier star with high [Sc/Fe] has also been found.We examine the extremely metal-poor tail of the HES metallicity distribution function (MDF). We suggest on the basis of comparison of our high resolution detailed abundance analyses with [Fe/H](HES) for stars in our sample that the MDF inferred from follow up spectra of the HES sample of candidate EMP stars is heavily contaminated for [Fe/H](HES) <\u22123 dex; many of the supposed EMP stars below that metallicity are of substantially higher Fe-metallicity, including most of the very C-rich stars, or are spurious objects.", "doi": "10.1063/1.2905516", "isbn": "978-0-7354-0509-7", "publisher": "American Institute of Physics", "place_of_publication": "Melville, NY", "publication_date": "2008-03-11", "pages": "118-121" }, { "id": "authors:1qgkk-31n26", "collection": "authors", "collection_id": "1qgkk-31n26", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160422-103841891", "type": "book_section", "title": "Magnesium Isotopes in Halo Stars", "book_title": "First stars III", "author": [ { "family_name": "Mel\u00e9ndez", "given_name": "Jorge", "orcid": "0000-0002-4933-2239", "clpid": "Mel\u00e9ndez-Jorge" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "O'Shea", "given_name": "Brian W.", "clpid": "O'Shea-Brian-W" }, { "family_name": "Heger", "given_name": "Alexander", "clpid": "Heger-Alexander" }, { "family_name": "Abel", "given_name": "Tom G.", "clpid": "Abel-Tom-G" } ], "abstract": "We have determined Mg isotope ratios in halo field dwarfs and giants in the globular cluster M71 based on high S/N high spectral resolution (R\u2009=\u200910^5) Keck HIRES spectra. Unlike previous claims of an important contribution from intermediate\u2010mass AGB stars to the Galactic halo, we find that our ^(26)Mg/^(24) Mg ratios can be explained by massive stars.", "doi": "10.1063/1.2905536", "isbn": "978-0-7354-0509-7", "publisher": "American Institute of Physics", "place_of_publication": "Melville, NY", "publication_date": "2008-03-11", "pages": "181-183" }, { "id": "authors:mqwgb-ftq71", "collection": "authors", "collection_id": "mqwgb-ftq71", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110322-113752943", "type": "book_section", "title": "Chemical Abundance Inhomogeneities in Globular Cluster Stars", "book_title": "Chemical Abundances and Mixing in Stars in the Milky Way and its Satellites", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Randich", "given_name": "Sofia", "clpid": "Randich-S" }, { "family_name": "Pasquini", "given_name": "Luca", "clpid": "Pasquini-L" } ], "abstract": "It is now clear that abundance variations from star-to-star among the light elements, particularly C, N, O, Na and Al, are ubiquitous within galactic globular clusters; they appear seen whenever data of high quality is obtained for a sufficiently large sample of stars within such a cluster. The correlations and anti-correlations among these elements and the range of variation of each element appear to be independent of stellar evolutionary state, with the exception that enhanced depletion of C and of O is sometimes seen just at the RGB tip. While the latter behavior is almost certainly due to internal production and mixing, the internal mixing hypothesis can now be ruled out for producing the bulk of the variations seen. We focus on the implications of our new data for any explanation invoking primordial variations in the proto-cluster or accretion of polluted material from a neighboring AGB star.", "doi": "10.1007/978-3-540-34136-9_38", "isbn": "3-540-34135-8", "publisher": "Springer", "place_of_publication": "New York, NY", "publication_date": "2006", "pages": "103-106" }, { "id": "authors:vaatc-hgp54", "collection": "authors", "collection_id": "vaatc-hgp54", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190522-103855423", "type": "book_section", "title": "The Frequency of Carbon Rich Stars Among Extremely Metal Poor Stars", "book_title": "From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Shectman", "given_name": "Stephen", "clpid": "Shectman-S-A" }, { "family_name": "Thompson", "given_name": "Ian", "clpid": "Thompson-I" }, { "family_name": "McWilliam", "given_name": "Andrew", "clpid": "McWilliam-A" }, { "family_name": "Christlieb", "given_name": "Norbert", "orcid": "0000-0002-4043-2727", "clpid": "Christlieb-N" }, { "family_name": "Mel\u00e9ndez", "given_name": "Jorge", "orcid": "0000-0002-4933-2239", "clpid": "Mel\u00e9ndez-J" }, { "family_name": "Zickgraf", "given_name": "Franz-Josef", "clpid": "Zickgraf-F-J" }, { "family_name": "Ramirez", "given_name": "Solange", "clpid": "Ram\u00edrez-S-V" }, { "family_name": "Swenson", "given_name": "Amber", "clpid": "Swenson-A" } ], "contributor": [ { "family_name": "Hill", "given_name": "V.", "clpid": "Hill-V" }, { "family_name": "Fran\u00e7ois", "given_name": "P.", "clpid": "Fran\u00e7ois-P" }, { "family_name": "Primas", "given_name": "F.", "clpid": "Primas-F" } ], "abstract": "We discuss the fraction of carbon stars (C-stars) and of C-enhanced stars among samples of candidate extremely metal poor (EMP: [Fe/H] \u2a7d\u22123.0 dex) stars selected from the Hamburg/ESO Survey (HES), obtaining a total for C-rich stars with [C/Fe] \u2a7e +1.0 dex of 14.4\u00b14%. We also present the key results of detailed abundance analyses of a sample of 14 C-stars selected in this way.", "doi": "10.1017/s1743921305005570", "isbn": "9780521851992", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2005-05", "pages": "213-218" }, { "id": "authors:4pe6w-3j818", "collection": "authors", "collection_id": "4pe6w-3j818", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904291", "type": "book_section", "title": "A Progress Report on the Caltech Faint Galaxy Redshift Survey", "book_title": "Deep Fields", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Cristiani", "given_name": "Stefano", "clpid": "Cristiani-S" }, { "family_name": "Renzini", "given_name": "Alvio", "clpid": "Renzini-A" }, { "family_name": "Williams", "given_name": "Robert E.", "clpid": "Williams-R-E" } ], "abstract": "I review recent progress on determining the SEDs and luminosity functions for galaxies in the large magnitude limited sample in the region of the HDF-North of the Caltech Faint Galaxy Redshift Survey.", "doi": "10.1007/10854354_10", "isbn": "3540427996", "publisher": "Springer-Verlag", "place_of_publication": "Berlin", "publication_date": "2003-09-26", "pages": "49-53" }, { "id": "authors:q5t33-g4t94", "collection": "authors", "collection_id": "q5t33-g4t94", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190522-081435717", "type": "book_section", "title": "Star Formation in the Hubble Deep Field North", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Avila-Reese", "given_name": "Vladimir", "clpid": "Avila-Reese-V" }, { "family_name": "Firmani", "given_name": "Claudio", "clpid": "Firmani-C" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Allen", "given_name": "Christine", "clpid": "Allen-C" } ], "abstract": "I am currently analyzing the emission line spectra of the 600 galaxies from the sample of Cohen et al. (2000) and Cohen (2001) in the region of the HDF-North with z < 1.5. A progress report on this effort of the Caltech Faint Galaxy Redshift Survey is presented.", "doi": "10.48550/arXiv.0207298", "publisher": "Universidad Nacional Aut\u00f3noma de M\u00e9xico", "publication_date": "2003" }, { "id": "authors:k2aje-3dv77", "collection": "authors", "collection_id": "k2aje-3dv77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181213-143633978", "type": "book_section", "title": "Imaging mass in three dimensions", "book_title": "Survey and Other Telescope Technologies and Discoveries", "author": [ { "family_name": "Wittman", "given_name": "D.", "clpid": "Wittman-D-E" }, { "family_name": "Margoniner", "given_name": "V. E.", "clpid": "Margoniner-V-E" }, { "family_name": "Tyson", "given_name": "J. A.", "clpid": "Tyson-J-A" }, { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Becker", "given_name": "A. C.", "clpid": "Becker-A-C" }, { "family_name": "Dell'Antonio", "given_name": "I. P.", "clpid": "Dell'Antonio-I-P" } ], "contributor": [ { "family_name": "Tyson", "given_name": "J. Anthony", "clpid": "Tyson-J-A" }, { "family_name": "Wolff", "given_name": "Sidney", "clpid": "Wolff-S" } ], "abstract": "We explore a possible \"killer app\" for the LSST and similar surveys: imaging mass in three dimensions. We describe its scientific importance, practical techniques for realizing it, the current state of the art and how it might scale to the LSST.", "doi": "10.1117/12.457372", "isbn": "9780819446152", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2002-12-24", "pages": "21-28" }, { "id": "authors:mqdak-r1x87", "collection": "authors", "collection_id": "mqdak-r1x87", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181213-143633825", "type": "book_section", "title": "Deep lens survey", "book_title": "Survey and Other Telescope Technologies and Discoveries", "author": [ { "family_name": "Wittman", "given_name": "D.", "clpid": "Wittman-D-M" }, { "family_name": "Tyson", "given_name": "J. A.", "clpid": "Tyson-J-A" }, { "family_name": "Dell'Antonio", "given_name": "I. P.", "clpid": "Dell'Antonio-I-P" }, { "family_name": "Becker", "given_name": "A. C.", "clpid": "Becker-A-C" }, { "family_name": "Margoniner", "given_name": "V. E.", "clpid": "Margoniner-V-E" }, { "family_name": "Cohen", "given_name": "J.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Norman", "given_name": "D.", "clpid": "Norman-D" }, { "family_name": "Loomba", "given_name": "D,", "clpid": "Loomba-D" }, { "family_name": "Squires", "given_name": "G.", "orcid": "0000-0002-1977-5717", "clpid": "Squires-G-K" }, { "family_name": "Wilson", "given_name": "G.", "orcid": "0000-0002-6572-7089", "clpid": "Wilson-G" }, { "family_name": "Stubbs", "given_name": "C.", "orcid": "0000-0003-0347-1724", "clpid": "Stubbs-C-W" }, { "family_name": "Hennawi", "given_name": "J.", "orcid": "0000-0002-7054-4332", "clpid": "Hennawi-J-F" }, { "family_name": "Spergel", "given_name": "D.", "orcid": "0000-0002-5151-0006", "clpid": "Spergel-D-N" }, { "family_name": "Boeshaar", "given_name": "P.", "clpid": "Boeshaar-P" }, { "family_name": "Clocchiatti", "given_name": "A.", "clpid": "Clocchiatti-A" }, { "family_name": "Hamuy", "given_name": "M.", "clpid": "Hamuy-M" }, { "family_name": "Bernstein", "given_name": "G.", "clpid": "Bernstein-G-M" }, { "family_name": "Gonzalez", "given_name": "A.", "orcid": "0000-0002-0933-8601", "clpid": "Gonzalez-A-H" }, { "family_name": "Guhathakurta", "given_name": "P.", "orcid": "0000-0001-8867-4234", "clpid": "Guhathakurta-P" }, { "family_name": "Hu", "given_name": "W.", "clpid": "Hu-W" }, { "family_name": "Seljak", "given_name": "U.", "clpid": "Seljak-U" }, { "family_name": "Zaritsky", "given_name": "D.", "orcid": "0000-0002-5177-727X", "clpid": "Zaritsky-D" } ], "contributor": [ { "family_name": "Tyson", "given_name": "J. Anthony", "clpid": "Tyson-J-A" }, { "family_name": "Wolff", "given_name": "Sidney", "clpid": "Wolff-S" } ], "abstract": "The Deep Lens Survey (DLS) is a deep BV Rz' imaging survey of seven 2\u00b0\u00d72\u00b0 degree fields, with all data to be made public. The primary scientific driver is weak gravitational lensing, but the survey is also designed to enable a wide array of other astrophysical investigations. A unique feature of this survey is the search for transient phenomena. We subtract multiple exposures of a field, detect differences, classify, and release transients on the Web within about an hour of observation. Here we summarize the scientific goals of the DLS, field and filter selection, observing techniques and current status, data reduction, data products and release, and transient detections. Finally, we discuss some lessons which might apply to future large surveys such as LSST.", "doi": "10.1117/12.457348", "isbn": "9780819446152", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2002-12-24", "pages": "73-82" }, { "id": "authors:mpp9b-z1x50", "collection": "authors", "collection_id": "mpp9b-z1x50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190524-104736397", "type": "book_section", "title": "Clustering in the Caltech Faint Galaxy Redshift Survey", "book_title": "Clustering at High Redshift", "author": [ { "family_name": "Cohen", "given_name": "Judith", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Mazure", "given_name": "A.", "clpid": "Mazure-A" }, { "family_name": "Le F\u00e8vre", "given_name": "O.", "clpid": "Le-F\u00e8vre-O" }, { "family_name": "Le Brun", "given_name": "V.", "clpid": "Le-Brun-V" } ], "abstract": "The Caltech Faint Galaxy Redshift Survey has collected \u223c2000 spectra taken with multi-slit masks using the Low Resolution Imaging Spectrograph at the Keck Observatory (Oke et al 1995) in two widely separated fields on the sky, each \u223c1 x 1 deg^2. Most of these objects are faint field galaxies; about 10% are Galactic stars and about 1% are broad-lined AGNs. \nI summarize the small scale clustering of this sample as well as the evidence in support of large scale structure.", "doi": "10.48550/arXiv.9910242", "isbn": "9781583810279", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2000", "pages": "314-318" }, { "id": "authors:bn6ke-bbe26", "collection": "authors", "collection_id": "bn6ke-bbe26", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190611-074244010", "type": "book_section", "title": "Variations in abundances among main sequence stars in M71", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Briley", "given_name": "Michael M.", "clpid": "Briley-M-M" } ], "contributor": [ { "family_name": "Noels", "given_name": "A.", "clpid": "Noels-A" }, { "family_name": "Magain", "given_name": "P.", "clpid": "Magain-P" }, { "family_name": "Caro", "given_name": "D.", "clpid": "Caro-D" }, { "family_name": "Jehin", "given_name": "E.", "clpid": "Jehin-E" }, { "family_name": "Parmentier", "given_name": "G.", "clpid": "Parmentier-G" }, { "family_name": "Thoul", "given_name": "A.", "clpid": "Thoul-A" } ], "abstract": "CH and CN variations are definitely present among the main sequence stars in a narrow range of luminosity just below the turnoff in the globular cluster stars. We show that the same set of C, N and O abundances that are used to fit the CN band in the CN-strong and CN-weak giants and subgiants in this cluster also successfully reproduce the behavior of the CH and CN molecular bands seen in the main sequence sample. This strongly suggests that the variations seen in M71 are primordial in origin. A hint of variation in the strength of the NaD lines is also seen in the main\nsequence sample. A range in Na abundance of about a factor of 3 is required to explain this. Strong Na among the main sequence stars appears to be correlated with strong CN, which is also characteristic\nof Na variations among red giants in globular clusters.", "publisher": "Universite de Li\u00e8ge", "publication_date": "2000" }, { "id": "authors:eynga-yc492", "collection": "authors", "collection_id": "eynga-yc492", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181211-082411138", "type": "book_section", "title": "Cosmological Parameters from the CERES Project", "book_title": "Cosmological Parameters and the Evolution of the Universe", "author": [ { "family_name": "Biggs", "given_name": "A.", "orcid": "0000-0002-1117-9961", "clpid": "Biggs-A-D" }, { "family_name": "Browne", "given_name": "I. W. A.", "clpid": "Browne-I-W-A" }, { "family_name": "Helbig", "given_name": "P.", "clpid": "Helbig-P" }, { "family_name": "Jackson", "given_name": "N. J.", "clpid": "Jackson-N-J" }, { "family_name": "King", "given_name": "L.", "clpid": "King-L" }, { "family_name": "Marlow", "given_name": "D. R.", "clpid": "Marlow-D-R" }, { "family_name": "McGuinness", "given_name": "A.", "clpid": "McGuinness-A" }, { "family_name": "Nair", "given_name": "S.", "clpid": "Nair-S" }, { "family_name": "Sykes", "given_name": "C. M.", "clpid": "Sykes-C-M" }, { "family_name": "Wilkinson", "given_name": "P. N.", "clpid": "Wilkinson-P-N" }, { "family_name": "Xanthopoulos", "given_name": "E.", "clpid": "Xanthopoulos-E" }, { "family_name": "de Bruyn", "given_name": "A. G.", "clpid": "de Bruyn-A-G" }, { "family_name": "Blandford", "given_name": "R.", "orcid": "0000-0002-1854-5506", "clpid": "Blandford-R-D" }, { "family_name": "Cohen", "given_name": "J.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Fassnacht", "given_name": "C.", "orcid": "0000-0002-4030-5461", "clpid": "Fassnacht-C-D" }, { "family_name": "Pearson", "given_name": "T.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Readhead", "given_name": "A.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Womble", "given_name": "D.", "clpid": "Womble-D-S" }, { "family_name": "Bremer", "given_name": "M.", "clpid": "Bremer-M-N" }, { "family_name": "Miley", "given_name": "G.", "clpid": "Miley-G-K" }, { "family_name": "Koopmans", "given_name": "L.", "orcid": "0000-0003-1840-0312", "clpid": "Koopmans-L-V-E" }, { "family_name": "Myers", "given_name": "S.", "clpid": "Myers-Steven-Theodore" }, { "family_name": "Patnaik", "given_name": "A.", "clpid": "Patnaik-A-R" } ], "contributor": [ { "family_name": "Sato", "given_name": "Katsuhiko", "clpid": "Sato-Katsuhiko" } ], "abstract": "[no abstract]", "doi": "10.1017/s0074180900132097", "isbn": "9780792354598", "publisher": "Kluwer", "place_of_publication": "Dordrecht", "publication_date": "1999", "pages": "64" }, { "id": "authors:x4g9d-qy024", "collection": "authors", "collection_id": "x4g9d-qy024", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190524-105032925", "type": "book_section", "title": "The Extremely Red Objects Found Thus Far in the Caltech Faint Galaxy Redshift Survey", "book_title": "Astrophysics with Infrared Surveys: A Prelude to SIRTF", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Hogg", "given_name": "David W.", "orcid": "0000-0003-2866-9403", "clpid": "Hogg-D-W" }, { "family_name": "Blandford", "given_name": "Roger", "orcid": "0000-0002-1854-5506", "clpid": "Blandford-R-D" }, { "family_name": "Pahre", "given_name": "Michael A.", "clpid": "Pahre-M-A" }, { "family_name": "Shopbell", "given_name": "Patrick L.", "clpid": "Shopbell-P-L" } ], "contributor": [ { "family_name": "Bicay", "given_name": "Michael D.", "clpid": "Bicay-M-D" }, { "family_name": "Beichman", "given_name": "C. A.", "clpid": "Beichman-C-A" }, { "family_name": "Cutri", "given_name": "Roc M.", "clpid": "Cutri-R-M" }, { "family_name": "Madore", "given_name": "Barry F.", "clpid": "Madore-B-F" } ], "abstract": "We discuss the very red objects found in the first field of the Caltech Faint Galaxy Redshift Survey, for which the observations and analysis are now complete. In this field, which is 15 arcmin^2 and at J005325+1234 there are 195 objects with K_s < 20 mag, of which 84% have redshifts. The sample includes 24 spectroscopically confirmed Galactic stars, 136 galaxies, three AGNs, and 32 objects without redshifts. \nAbout 10% of the sample has (R\u2212K) \u2265 5 mag. Four of these objects have redshifts, with 0.78 \u2264 z \u2264 1.23. Three of these are based on absorption features in the mid-UV, while the lowest redshift object shows the standard features near 4000\u00c5. Many of the objects still without redshifts have been observed spectroscopically, and no emission lines were seen in their spectra. We believe they are galaxies with z \u223c1\u22121.5 that are red due to their age and stellar content and not to some large amount of internal reddening from dust. \nAmong the many other results from this survey of interest here is a determination of the median extinction in the mid-UV for objects with strong emission line spectra at z \u223c1\u22121.3. The result is extinction by a factor of \u223c2 at 2400 \u00c5.", "doi": "10.48550/arXiv.9808343", "isbn": "9781583810019", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1999", "pages": "47-50" }, { "id": "authors:0n6ps-89b17", "collection": "authors", "collection_id": "0n6ps-89b17", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190604-144842812", "type": "book_section", "title": "The blue channel of the Keck low-resolution imaging spectrometer", "book_title": "Optical Astronomical Instrumentation", "author": [ { "family_name": "McCarthy", "given_name": "James K.", "clpid": "McCarthy-J-K" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Butcher", "given_name": "Brad", "clpid": "Butcher-B" }, { "family_name": "Cromer", "given_name": "John", "clpid": "Cromer-J-L" }, { "family_name": "Croner", "given_name": "Ernest", "clpid": "Croner-E-E" }, { "family_name": "Douglas", "given_name": "Bill", "clpid": "Douglas-W-R-Jr" }, { "family_name": "Goeden", "given_name": "Rich", "clpid": "Goeden-R-M" }, { "family_name": "Grewal", "given_name": "Tony", "clpid": "Grewal-T" }, { "family_name": "Lu", "given_name": "Barry", "clpid": "Lu-Barry" }, { "family_name": "Petrie", "given_name": "Hal", "clpid": "Petrie-H-L" }, { "family_name": "Weng", "given_name": "Tianxiang", "clpid": "Weng-Tianxiang" }, { "family_name": "Weber", "given_name": "Bob", "clpid": "Weber-B" }, { "family_name": "Koch", "given_name": "Donald", "clpid": "Koch-D-G" }, { "family_name": "Rodgers", "given_name": "J. Michael", "clpid": "Rodgers-J-M" } ], "contributor": [ { "family_name": "D'Odorico", "given_name": "Sandro", "clpid": "D'Odorico-S" } ], "abstract": "This paper summarizes the optical, mechanical, electrical, and software design of LRIS-B, the blue channel of the Keck Low Resolution and Imaging Spectrograph. The LRIS-B project will shortly be completing the existing LRIS instrument through the addition of dichroic beamsplitters, grisms to disperse light on the blue channel, broad-band u, B, and V photometric filters, a blue and near-UV transmitting camera lens, and a large format blue-sensitive CCD detector. LRIS-B will also introduce piezoelectric xy-actuation of the CCD detector inside its Dewar, in order to compensate for flexure in the existing instrument; ultimately the red-side CCD detector will be similarly equipped, its PZT xy-stage being independently programmed. The optical design of the LRIS-B camera uses only fused silica and calcium fluoride elements, and includes a decentered meniscus element to compensate for coma introduced by the LRIS off-axis paraboloid collimator. The design of the blue channel grisms have been optimized for maximum blaze efficiency, the highest dispersion grism having a groove density of 1200 gr/mm. Optical elements not in use at any given time will be stowed in carousels externally mounted to the instrument sidewalls. The entire instrument is designed to permit remote operation.", "doi": "10.1117/12.316831", "isbn": "9780819428028", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1998-07-09", "pages": "81-92" }, { "id": "authors:7b35q-gse32", "collection": "authors", "collection_id": "7b35q-gse32", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-152854352", "type": "book_section", "title": "A Progress Report on the Caltech Deep Redshift Survey", "book_title": "The Young Universe: Galaxy Formation and Evolution at Intermediate and High Redshift", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "D'Odorico", "given_name": "S.", "clpid": "D'Odorico-S" }, { "family_name": "Fontana", "given_name": "A.", "clpid": "Fontana-A" }, { "family_name": "Giallongo", "given_name": "E.", "clpid": "Giallongo-E" } ], "abstract": "The Caltech Deep Redshift Survey (CDRS) has been working\nin two fields. More than 1000 redshifts for faint field galaxies in these two fields are in hand. Our discovery of strong redshift clustering at high z is now amply confirmed by the large data set in hand. Many redshift peaks, with a typical, but non-periodic, spacing of \u2248100 h^(-1) Mpc, are seen in the HDF data. We have carried out a preliminary determination of the luminosity function for galaxies, as well as an analysis of the star formation rate as a function of time.\nThe two point correlation function for galaxies has also been derived. The spatial analysis is directly calculated using the statistics of pairs. A byproduct of this analysis is the measurement of the deviation from smooth Hubble flow (\u2248300 km/sec in the rest frame) at z \u2248 0.6. The spectral analysis is in a very preliminary state. Thus far we have established that the emission line ratios for our sample indicate photoionization by starlight and do not provide any evidence for a contribution by a harder ionizing flux (i.e. AGNs).", "isbn": "9781886733664", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1998", "pages": "420-427" }, { "id": "authors:9yj47-chq14", "collection": "authors", "collection_id": "9yj47-chq14", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-151516596", "type": "book_section", "title": "Remote Observing with the Keck Telescope: ATM Networks and Satellite Systems", "book_title": "Astronomical Data Analysis Software and Systems VII", "author": [ { "family_name": "Shopbell", "given_name": "P. L.", "clpid": "Shopbell-P-L" }, { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Bergman", "given_name": "L.", "clpid": "Bergman-L-A" } ], "abstract": "As a technical demonstration project for the NASA Advanced Communications Technology Satellite (ACTS), we have implemented remote observing on the 10-meter Keck II telescope on Mauna Kea from the Caltech campus in Pasadena. The data connection consists of ATM networks in Hawaii and California, running at OC-1 speeds (45 Mbit/sec), and high data rate (HDR) satellite antennae at JPL in Pasadena and Tripler Army Medical Center in Honolulu. The ACTS network is being used to enable true remote observing, as well as remote eavesdropping. The software environment is identical to that used for on-site observing at the Keck telescope, with the added benefit of the software, personnel, and other facilities provided by observing in a local environment. In this paper, we describe our high-speed remote observing network, assess the network's level of performance, and summarize the benefits and difficulties encountered in this project.", "isbn": "9781886733657", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1998", "pages": "348-351" }, { "id": "authors:stn76-t6869", "collection": "authors", "collection_id": "stn76-t6869", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190603-153225613", "type": "book_section", "title": "Remote observing with the Keck Telescope from California using NASA's ACTS satellite", "book_title": "Telescope Control Systems II", "author": [ { "family_name": "Shopbell", "given_name": "P. L.", "clpid": "Shopbell-P-L" }, { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Bergman", "given_name": "L.", "clpid": "Bergman-L-A" } ], "contributor": [ { "family_name": "Lewis", "given_name": "Hilton", "clpid": "Lewis-H-A" } ], "abstract": "As a technical demonstration project for the NASA Advanced Communications Technology Satellite (ACTS), we have implemented remote observing on the 10-meter Keck II telescope on Mauna Kea in Hawaii from the California Institute of Technology campus in Pasadena. The data connection consists of ATM networks in Hawaii and California, running at OC-1 speeds (51 Mbit/sec) through optical fiber, and high data rate (HDR) satellite antennae at JPL in Pasadena and at the Tripler Army Medical Center in Honolulu. The ACTS network provides sufficient bandwidth to enable true remote observing, with a software environment identical to that used for on-site observing. \n\nIn this paper, we demonstrate that while the satellite link introduces a number of difficulties and decreases overall reliability of the system, remote observing is not only feasible, but provides several important advantages over standard observing paradigms. Benefits include involving more members of observing teams while decreasing expenses, enhancing real-time data analysis of observations by persons not subject to altitude-related conditions, and providing facilities, expertise, and personnel not normally available at the observing site. Although the current bandwidth of the public Internet is insufficient for true remote observing, we nevertheless anticipate a growing role for remote observing techniques, particularly as high-speed terrestrial networking paradigms, such as ATM, become more commonly available.", "doi": "10.1117/12.278835", "isbn": "9780819425348", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1997-09-18", "pages": "209-220" }, { "id": "authors:e3cf0-15t24", "collection": "authors", "collection_id": "e3cf0-15t24", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-150033937", "type": "book_section", "title": "A High Speed Network for Remote Observing from Caltech with the Keck Telescope", "book_title": "Astronomical Data Analysis Software and Systems V", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Bergman", "given_name": "L.", "clpid": "Bergman-L-A" }, { "family_name": "Shopbell", "given_name": "P. L.", "clpid": "Shopbell-P-L" } ], "contributor": [ { "family_name": "Jacoby", "given_name": "George H.", "clpid": "Jacoby-G-H" }, { "family_name": "Barnes", "given_name": "Jeannette", "clpid": "Barnes-J" } ], "abstract": "We are setting up a high speed (DS3) ATM network running from the dome of the 10-meter Keck Telescope on the summit of Mauna Kea in Hawaii to the Caltech campus in Pasadena, California. This network will be used to support remote observing, remote diagnostics of problems, remote software development, and other related tasks. We discuss the motivation for this effort, the network architecture, and the current status of this project.", "isbn": "978-1-58381-437-6", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1996", "pages": "376-379" }, { "id": "authors:tx68z-gv578", "collection": "authors", "collection_id": "tx68z-gv578", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-145022397", "type": "book_section", "title": "A Summary of Ongoing Work at the Keck Telescope on Gravitational Lensing and on Distant Galaxies", "book_title": "Clusters, Lensing, and the Future of the Universe", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Trimble", "given_name": "Virginia", "clpid": "Trimble-V-L" }, { "family_name": "Reisenegger", "given_name": "Andreas", "clpid": "Reisenegger-A" } ], "abstract": "I present a summary of recent scientific projects relevant to the areas being discussed at this conference that have been or are in the process of being carried out at the Keck telescope by astronomers from the California Institute of Technology. Note that in most cases these are team projects, and many people are involved. Among the highlights thus far in the area of gravitational lensing are the detection of an emission line in the lens B0218+357 implying, if its identification as Mgll is correct, a redshift of 0.95, and the detection of a redshift of 0.53 for one of the arcs in the X-ray emitting cluster of galaxies MS 0440+0204. Highlights in the area of\ndistant galaxies include the deepest published optical and infrared counts, reaching to K = 24.5 mag and to R \u2248 27 mag. The first results from a redshift survey of faint field galaxies which will eventually reach to K \u2264 20 mag are also shown.", "isbn": "9781886733091", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1996", "pages": "68-75" }, { "id": "authors:wgfwn-nm656", "collection": "authors", "collection_id": "wgfwn-nm656", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161905051", "type": "book_section", "title": "The Globular Cluster System of M87", "book_title": "Stellar Populations", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "van der Kruit", "given_name": "P. C.", "clpid": "van-der-Kruit-P-C" }, { "family_name": "Gilmore", "given_name": "C.", "clpid": "Gilmore-C" } ], "abstract": "We have begun a program with the Low Resolution Imaging Spectrograph, operating with 30 multi-slits per exposure (Oke et al 1994, Cohen et al 1993) on the ten-meter W. M. Keck telescope located on Mauna Kea, Hawaii to observe the globular cluster systems of the Virgo ellipticals. We expect to learn about the dark matter content of galaxy halos, the formation of these halos and their cluster systems, possibly the formation of the galaxy's themselves, the interaction of the cluster system with the galaxy's gravitational potential (i.e. rotation and spinup), and the homogeneity of chemical evolution in various places. The metallicity of the globular clusters versus the metallicity of the underlying galaxy can also by analyzed. In addition the dynamics (i.e. in practice, the rotation and velocity dispersion) of the halo of the parent galaxy versus the globular cluster system can be determined.", "doi": "10.1007/978-94-011-0125-7_111", "isbn": "9780792335382", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1995", "pages": "441-442" }, { "id": "authors:njdyt-39638", "collection": "authors", "collection_id": "njdyt-39638", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161019-074955837", "type": "book_section", "title": "Low-Resolution Imaging Spectrometer for the Keck Telescope", "book_title": "Instrumentation in Astronomy VIII", "author": [ { "family_name": "Oke", "given_name": "J. Beverly", "clpid": "Oke-J-B" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Carr", "given_name": "Michael M.", "clpid": "Carr-M-M" }, { "family_name": "Dingiziam", "given_name": "Arsham", "clpid": "Dingiziam-A" }, { "family_name": "Harris", "given_name": "Frederick H.", "clpid": "Harris-F-H" }, { "family_name": "Lucinio", "given_name": "Richard", "clpid": "Lucinio-R" }, { "family_name": "Labrecque", "given_name": "S.", "clpid": "Labrecque-S" }, { "family_name": "Schaal", "given_name": "W. A.", "clpid": "Schaal-W-A" }, { "family_name": "Southard", "given_name": "S., Jr.", "clpid": "Southard-S-Jr" } ], "contributor": [ { "family_name": "Crawford", "given_name": "D. I.", "clpid": "Crawford-D-I" }, { "family_name": "Craine", "given_name": "Eric R.", "clpid": "Craine-E-R" } ], "abstract": "The Low Resolution Imaging Spectrometer is designed for use at the Cassegrain focus of the Keck 10-m telescope. It provides the capability of acquiring low resolution (R equals 1000 to 5000) digital spectra, as well as 6 X 8 arc-minute moderately high spatial resolution (4.65 pixels/arc-second) direct images. Spectroscopy can be carried out with single slits which are 3 arc-minutes long. In addition punched multi-slits can also be employed which allow for the acquisition of at least forty spectra simultaneously. Since the instrument is designed to be as efficient as possible, it is a double spectrograph, with a dichroic splitting the blue and red light into separate optical paths after the collimator. Only the red side has been constructed thus far. With a 2048 by 2048 thinned Tektronix CCD as the detector the total efficiency of the red side at the peak of the grating blaze is predicted to be nearly 40%. Results of the commissioning observing runs will be described.", "doi": "10.1117/12.176745", "isbn": "0-8194-1493-X", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1994-06-01", "pages": "178-184" }, { "id": "authors:ha7jp-3c877", "collection": "authors", "collection_id": "ha7jp-3c877", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161905136", "type": "book_section", "title": "Infrared Photometry of Metal Rich Galactic Globular Clusters", "book_title": "Infrared Astronomy with Arrays: the Next Generation", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Sleeper", "given_name": "C.", "clpid": "Sleeper-C" } ], "contributor": [ { "family_name": "McLean", "given_name": "Ian S.", "clpid": "McLean-I-S" } ], "abstract": "We describe the results of a program of infrared photometry using an array detector carried out at the Las Campanas Observatory on a sample of very metal rich galactic globular clusters. We have found that the giant branches of most of these clusters show a spread in various colors which is due to patchy interstellar absorption. Strong limits can be derived on the metallicity spread within these clusters by analyzing the spread of the giant branch at a given K magnitude as a function of color used.", "doi": "10.1007/978-94-011-1070-9_20", "isbn": "9789401044660", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1994", "pages": "93-94" }, { "id": "authors:782xa-p7569", "collection": "authors", "collection_id": "782xa-p7569", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-144040919", "type": "book_section", "title": "The Software for the LRIS on the Keck 10-Meter Telescope", "book_title": "Astronomical Data Analysis Software and Systems III", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Cromer", "given_name": "J. L.", "clpid": "Cromer-J-L" }, { "family_name": "Southard", "given_name": "S., Jr.", "clpid": "Southard-S-Jr" }, { "family_name": "Clowe", "given_name": "D.", "clpid": "Clowe-D-I" } ], "contributor": [ { "family_name": "Crabtree", "given_name": "Dennis R.", "clpid": "Crabtree-D-R" }, { "family_name": "Hanisch", "given_name": "R. J.", "clpid": "Hanisch-R-J" }, { "family_name": "Barnes", "given_name": "Jeannette", "clpid": "Barnes-J" } ], "abstract": "We discuss the software for the Low Resolution and Imaging Spectrograph, one of the first light instruments built for the Keck 10-meter telescope. Details of the CCD detector readout scheme, the motor control system, the user interface, the astrometric preparatory software, etc., are given.", "isbn": "9780937707807", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1994" }, { "id": "authors:fn34h-q4y28", "collection": "authors", "collection_id": "fn34h-q4y28", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-140917632", "type": "book_section", "title": "Baade-Wesselink Distances to M5 and M92", "book_title": "Structure and Dynamics of Globular Clusters", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Djorgovski", "given_name": "S. G.", "clpid": "Djorgovski-S-G" }, { "family_name": "Meylan", "given_name": "Georges", "clpid": "Meylan-G" }, { "family_name": "King", "given_name": "Ivan", "clpid": "King-I-R" } ], "abstract": "A Baade-Wesselink analysis has been performed using new optical and infrared photometry of four RR Lyrae variables in the globular cluster M5 and two in M92. We obtain a distance to M5 of 6.9 \u00b1 0.45 kpc and to M92 of 7.85 \u00b1 0.45 kpc, with a 0.3 kpc additional systematic uncertainty. These results are in excellent agreement with the previously published distances, based on matching the globular cluster main sequence to that defined by the field subdwarfs of known distance.", "isbn": "9780937707692", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1993", "pages": "309-310" }, { "id": "authors:6rgpv-tgf75", "collection": "authors", "collection_id": "6rgpv-tgf75", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-135701573", "type": "book_section", "title": "The M31 Globular Clusters in the Infrared", "book_title": "The Globular Cluster-Galaxy Connection", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Smith", "given_name": "Graeme H.", "clpid": "Smith-G-H" }, { "family_name": "Brodie", "given_name": "Jean P.", "clpid": "Brodie-J-P" } ], "abstract": "We review the infrared observations, both photometric and spectroscopic, of the globular clusters of M31. As a preliminary step, we summarize the observations in the infrared of individual stars in galactic globular clusters, then the observations of the integrated light of galactic globular clusters as well as the models that are used to interpret their properties. Another area that is\ndiscussed is the infrared observations of clusters in the Magellanic Clouds, their interpretation, and how they differ from galactic globular clusters. We also compare the observations of all these with the trends shown by normal elliptical galaxies.", "isbn": "9780937707678", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1993", "pages": "438-447" }, { "id": "authors:wbs0p-fnq54", "collection": "authors", "collection_id": "wbs0p-fnq54", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-134324219", "type": "book_section", "title": "Baade-Wesselink Distances to MS and M92", "book_title": "The Globular Cluster-Galaxy Connection", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Smith", "given_name": "Graeme H.", "clpid": "Smith-G-H" }, { "family_name": "Brodie", "given_name": "Jean P.", "clpid": "Brodie-J-P" } ], "abstract": "A Baade-Wesselink analysis has been performed using new optical and infrared photometry of four RR Lyrae variables in the globular cluster M5 and two in M92. We obtain a distance to M5 of 6.9 \u00b1 0.45 kpc and to M92 of 7.85 \u00b1 0.45 kpc, with a 0.3 kpc additional systematic uncertainty. These results are in excellent agreement with the previously published distances, based on matching the globular cluster main sequence to that defined by the field subdwarfs of known distance.", "isbn": "9780937707678", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1993", "pages": "78-79" }, { "id": "authors:01c0x-xfp89", "collection": "authors", "collection_id": "01c0x-xfp89", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-133424788", "type": "book_section", "title": "The tidal radii of globular clusters in M31", "book_title": "The formation and evolution of star clusters", "author": [ { "family_name": "Cohen", "given_name": "Judith", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Freeman", "given_name": "Kenneth", "clpid": "Freeman-K-A" } ], "contributor": [ { "family_name": "Janes", "given_name": "Kenneth", "clpid": "Janes-K" } ], "abstract": "We have determined tidal radii for 30 globular clusters in the halo of M31 from deep direct images. Although the uncertainty of each individual measurement is large, in the mean the tidal radii suggest that the M31 globular clusters have orbital eccentricities and mass-to-light ratios that are very similar to those of Galactic globular clusters.", "isbn": "9780937707326", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1991", "pages": "377-380" }, { "id": "authors:n9b47-gvb02", "collection": "authors", "collection_id": "n9b47-gvb02", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904112", "type": "book_section", "title": "The Photometric Accuracy of Astronomical Images Restored with the MEMSYS3 Code", "book_title": "Maximum Entropy and Bayesian Methods", "author": [ { "family_name": "Cohen", "given_name": "J. G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Grandy", "given_name": "W. T., Jr.", "clpid": "Grandy-W-T-Jr" }, { "family_name": "Schick", "given_name": "L. H.", "clpid": "Schick-L-H" } ], "abstract": "After reviewing the causes of blur in astronomical images obtained with optical telescopes, both ground based instruments and the Hubble Space Telescope, simulations are described which test the photometric accuracy of the maximum entropy image restoration algorithm used in the code Memsys3 version 2. It is found that at the faintest brightness levels, while the code can recover blurred out point sources, they are recovered systematically too faint. The size of the photometric error depends on the brightness of the source (relative to the noise of the background) and the crowding of the field. At present, the optimum technique to apply to blurred images of crowded fields where most of the sources are point sources seems to be to use a restored image to generate the list of objects, then feed this into a standard point spread function fitting code and use this on the original blurred frame. In that manner, the most crowded fields can be analyzed without losing photometric accuracy.", "doi": "10.1007/978-94-011-3460-6_6", "isbn": "9789401055314", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1991", "pages": "59-65" }, { "id": "authors:5f23w-0wk25", "collection": "authors", "collection_id": "5f23w-0wk25", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-132642801", "type": "book_section", "title": "Structural Parameters for Globular Clusters in M 31", "book_title": "CCDs in Astronomy. II. New Methods and Applications of CCD Technology", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Philip", "given_name": "A. G. Davis", "clpid": "Philip-A-G-D" }, { "family_name": "Hayes", "given_name": "D. S.", "clpid": "Hayes-D-S" }, { "family_name": "Adelman", "given_name": "S. J.", "clpid": "Adelman-S-J" } ], "abstract": "After a review of existing data on structural parameters for globular clusters, we present new measurements of tidal radii for 30 globular clusters in M 31. These measurements are consistent with the globular clusters in M 31 having the same mean M/L ratio as those in the Galaxy.", "isbn": "9780933485129", "publisher": "L. Davis Press", "place_of_publication": "Schenectady, NY", "publication_date": "1990", "pages": "167-176" }, { "id": "authors:txmjr-1xk54", "collection": "authors", "collection_id": "txmjr-1xk54", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904378", "type": "book_section", "title": "The Globular Cluster System of M87", "book_title": "The Harlow-Shapley Symposium on Globular Cluster Systems in Galaxies", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Grindlay", "given_name": "Jonathan E.", "clpid": "Grindlay-J-E" }, { "family_name": "Davis Philip", "given_name": "A. G.", "clpid": "Davis-Philip-A-G" } ], "abstract": "Long exposures with the 4-Shooter at the Cassegrain focus of the 200-inch telescope at Palomar Observatory have been obtained for M87 (and two other giant ellipticals in Virgo). Ellipse fitting with a code specially developed to reject point sources has been carried out to determine the surface brightness in various bandpasses of the underlying galaxy. The color gradients in the galaxy are quite small over the entire regime between 2 and 350 arc-sec from the nucleus of M87. Also I find that there is no difference between the ellipse parameters (position angle and eccentricity) derived in the various colors, i.e. the isochromes and the isophotes coincide. Details of the study of the halo of M87 are described in a paper submitted to the Astronomical Journal.", "doi": "10.1007/978-94-015-1104-9_125", "isbn": "9789027726650", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1988", "pages": "605-606" }, { "id": "authors:rg6hm-4zq12", "collection": "authors", "collection_id": "rg6hm-4zq12", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904470", "type": "book_section", "title": "The FIGARO Package for Astronomical Data Analysis", "book_title": "Instrumentation for Ground-Based Optical Astronomy: Present and Future", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Robinson", "given_name": "Lloyd B.", "clpid": "Robinson-L-B" } ], "abstract": "The FIGARO software package was originally written in the early 1980s by Keith Shortridge for analysis of data from Palomar Observatory. It is currently maintained by Shortridge from the Anglo-Australian Observatory. In the intervening years, FIGARO has grown rich in applications and has dispersed widely through the world from its Caltech base.", "doi": "10.1007/978-1-4612-3880-5_43", "isbn": "9781461283874", "publisher": "Springer", "place_of_publication": "New York, NY", "publication_date": "1988", "pages": "448-457" }, { "id": "authors:hnnxn-3ts44", "collection": "authors", "collection_id": "hnnxn-3ts44", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190531-091631410", "type": "book_section", "title": "Multiple Object Fiber Optics Spectrograph Feed For The Hale Telescope", "book_title": "Instrumentation in Astronomy IV", "author": [ { "family_name": "Tubbs", "given_name": "Eldred F.", "clpid": "Tubbs-E-F" }, { "family_name": "Goss", "given_name": "Willis C.", "clpid": "Goss-W-C" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Crawford", "given_name": "David L.", "clpid": "Crawford-D-L" } ], "abstract": "A preliminary design of a fiber-optics feed for the prime-focus spectrograph of the Hale telescope using computer controlled movable fiber has been completed and a test of a proto-type configuration carried out. The complete design will divide a 76mm square field into 10 strips and will place two movable fibers in each strip. The fiber pickups, which are moved by stepper-motor driven lead screws, may be placed anywhere in the strip subject to the limitation that they not pass each other. The prototype consisted of a single strip with two fibers operated with manual input to the stepper motors. In tests performed at the 5 meter Hale telescope in April of 1981 spec-tra of two bright 0 stars (B = 8.5 mag) separated by 5 arc minutes were photographed with a 3 minute exposure using a 1200 line/mm grating and unbaked 103a0 plates. The performance of the prototype configuration was within a factor of two of the unmodified prime-focus spec-trograph indicating a potential for a ten-fold increase in the effective utilization of the telescope for spectrographic survey work when fitted with the 20-fiber feed.", "doi": "10.1117/12.933468", "isbn": "9780892523665", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1982-11-16", "pages": "289-295" }, { "id": "authors:y3nkg-9yh57", "collection": "authors", "collection_id": "y3nkg-9yh57", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904668", "type": "book_section", "title": "Observed Bolometric Luminosities of Carbon Stars", "book_title": "Physical Processes in Red Giants", "author": [ { "family_name": "Frogel", "given_name": "Jay A.", "clpid": "Frogel-J-A" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" }, { "family_name": "Elias", "given_name": "Jonathan H.", "clpid": "Elias-J-H" } ], "contributor": [ { "family_name": "Iben", "given_name": "Icko, Jr.", "clpid": "Iben-I-Jr" }, { "family_name": "Renzini", "given_name": "Alvio", "clpid": "Renzini-A" } ], "abstract": "To the best of our knowledge, most carbon stars are cool stars on their second ascent of the giant branch, i.e. the asymptotic giant branch. By some means they have mixed nuclear processed, carbon enriched material to their surfaces and probably have luminosities that are greater than those that mark the termination point of first time evolution up the giant branch, i.e. the location of the core helium flash. Observational and theoretical evidence for this picture may be found in Iben and Truran (1978), Renzini and Voli (1980), Scalo (1976), Richer, Olander and Westerlund (1979), and earlier references these authors cite.", "doi": "10.1007/978-94-009-8492-9_15", "isbn": "9789400984943", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication_date": "1981", "pages": "159-164" }, { "id": "authors:t4kb6-gwe37", "collection": "authors", "collection_id": "t4kb6-gwe37", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904568", "type": "book_section", "title": "Globular Cluster Giant Branches and the Helium Flash: A Comparison between Observation and Theory", "book_title": "Physical Processes in Red Giants", "author": [ { "family_name": "Frogel", "given_name": "Jay A.", "clpid": "Frogel-J-A" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Iben", "given_name": "Icko, Jr.", "clpid": "Iben-I-Jr" }, { "family_name": "Renzini", "given_name": "Alvio", "clpid": "Renzini-A" } ], "abstract": "Four years ago we began a study of globular cluster giant stars in the infrared. The first part of this program, the measurement of the 1.2\u20132.2 \u00b5m energy distributions with the use of broad band filters and the determination of the strengths of CO and H2O absorption in the stars has been published, or will soon appear in press. M3, M13, and M92 are discussed in Cohen, Frogel, and Persson (1978, hereafter CFP); M71 in Frogel, Persson, and Cohen (1979); \u03c9 Centauri in Persson et al. (1980); Pal 12 in Cohen et al. (1980); 47 Tucanae in Frogel, Persson, and Cohen (1981, hereafter FPC1); and NGC 3201 in Da Costa, Frogel, and Cohen (1981). We now have in hand similar data for 167 stars in 11 additional clusters: NGC 288, 362, 5904 (M5), 6121 (M4), 6352, 6397, 6637 (M69), 6656 (M22), 6752, 7006, and 7078 (M15) (Frogel, Persson, and Cohen 1982, hereafter FPC2). Pilachowski (1978) has also published data on several of these clusters and M10. With a rather complete sample of cluster types, we can proceed to examine how physical quantities derivable from infrared data vary from cluster to cluster. Furthermore it should be possible to establish \"benchmarks\" against which theoretical models of stellar atmospheres and evolutionary tracks can be tested.", "doi": "10.1007/978-94-009-8492-9_6", "isbn": "9789400984943", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1981", "pages": "55-62" }, { "id": "authors:cjeje-n0y04", "collection": "authors", "collection_id": "cjeje-n0y04", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904766", "type": "book_section", "title": "Diffuse Interstellar Band Formation in Dense Clouds", "book_title": "Solid State Astrophysics", "author": [ { "family_name": "Snow", "given_name": "Theodore P., Jr.", "clpid": "Snow-T-P-Jr" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" } ], "contributor": [ { "family_name": "Wickramasinghe", "given_name": "N. C.", "clpid": "Wickramasinghe-N-C" }, { "family_name": "Morgan", "given_name": "D. J.", "clpid": "Morgan-D-J" } ], "abstract": "Measurements of the strengths of the diffuse interstellar bands at 4430, 5780 and 5797 \u00c5 show that the bands tend to be weak with respect to extinction in dense interstellar clouds. Data on 10 stars in the Q Ophiuchi cloud complex show further that the diffuse band-producing efficiency of the grains decreases systematically with increasing grain size. It is concluded that the diffuse bands are not formed in the mantles which accrete on the grains in interstellar clouds, but that they could be produced in the cores of grains or in some molecular species.", "doi": "10.1007/978-94-010-1884-5_5", "isbn": "9789401018869", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1976", "pages": "33-38" } ]