Submitted - 2201.05603.pdf
", "abstract": "We determine the low-redshift X-ray luminosity function (XLF), active black hole mass function (BHMF), and Eddington-ratio distribution function (ERDF) for both unobscured (Type 1) and obscured (Type 2) active galactic nuclei (AGN) using the unprecedented spectroscopic completeness of the BAT AGN Spectroscopic Survey (BASS) data release 2. In addition to a straightforward 1/Vmax approach, we also compute the intrinsic distributions, accounting for sample truncation by employing a forward modeling approach to recover the observed BHMF and ERDF. As previous BHMFs and ERDFs have been robustly determined only for samples of bright, broad-line (Type 1) AGNs and/or quasars, ours is the first directly observationally constrained BHMF and ERDF of Type 2 AGN. We find that after accounting for all observational biases, the intrinsic ERDF of Type 2 AGN is significantly skewed towards lower Eddington ratios than the intrinsic ERDF of Type 1 AGN. This result supports the radiation-regulated unification scenario, in which radiation pressure dictates the geometry of the dusty obscuring structure around an AGN. Calculating the ERDFs in two separate mass bins, we verify that the derived shape is consistent, validating the assumption that the ERDF (shape) is mass independent. We report the local AGN duty cycle as a function of mass and Eddington ratio, by comparing the BASS active BHMF with the local mass function for all SMBH. We also present the log N-log S of Swift-BAT 70-month sources.", "date": "2022-01-14", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20220119-234014000", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220119-234014000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "80NSSC19K0580" }, { "agency": "NSF", "grant_number": "AST-1554584" }, { "agency": "Israel Science Foundation", "grant_number": "1849/19" }, { "agency": "European Research Council (ERC)", "grant_number": "950533" }, { "agency": "NASA", "grant_number": "NNH16CT03C" }, { "agency": "NSF", "grant_number": "AST-1715512" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "11190831" }, { "agency": "BASAL-CATA", "grant_number": "AFB-170002" }, { "agency": "Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID)", "grant_number": "FB210003" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1200495" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "1190818" }, { "agency": "Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID)", "grant_number": "ACT172033" }, { "agency": "Agencia Nacional de Investigaci\u00f3n y Desarrollo (ANID)", "grant_number": "NCN19_058" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "ICN12_009" }, { "agency": "National Research Foundation of Korea", "grant_number": "NRF-2020R1C1C1005462" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18K13584" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20H01939" }, { "agency": "NSF", "grant_number": "PHY-1607611" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.2201.05603", "primary_object": { "basename": "2201.05603.pdf", "url": "https://authors.library.caltech.edu/records/rqg6n-rqr66/files/2201.05603.pdf" }, "pub_year": "2022", "author_list": "Ananna, Tonima Tasnim; Weigel, Anna K.; et al." }, { "id": "https://authors.library.caltech.edu/records/p7s73-fem72", "eprint_id": 113005, "eprint_status": "archive", "datestamp": "2023-08-20 06:11:57", "lastmod": "2025-06-30 18:18:09", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Greffe-Timoth\u00e9e", "name": { "family": "Greffe", "given": "Timothee" } }, { "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "Roger" }, "orcid": "0000-0001-7062-9726" }, { "id": "Sherman-Myles", "name": { "family": "Sherman", "given": "Myles" } }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona" }, "orcid": "0000-0002-4226-8959" }, { "id": "Earnshaw-Hannah-P", "name": { "family": "Earnshaw", "given": "Hannah" }, "orcid": "0000-0001-5857-5622" }, { "id": "Grefenstette-Brian-W", "name": { "family": "Grefenstette", "given": "Brian" }, "orcid": "0000-0002-1984-2932" }, { "id": "Hennessy-John", "name": { "family": "Hennessy", "given": "John" }, "orcid": "0000-0002-0135-0219" }, { "id": "Nikzad-Shouleh", "name": { "family": "Nikzad", "given": "Shouleh" } } ] }, "title": "Characterization of Low Light Performance of a CMOS sensor for Ultraviolet Astronomical Applications", "ispublished": "unpub", "full_text_status": "public", "keywords": "CMOS, SRI mK\u2002nK, ultraviolet, dark current, glow suppression, dual-gain", "note": "Attribution 4.0 International (CC BY 4.0).\n\nWe thank the SRI team for packaging multiple detectors and performing screening tests, and for their advice during our detector characterization effort. We acknowledge the support of JPL and Caltech's President and Director's Research and Development Fund (PDRDF Program). We also gratefully acknowledge the collaborative agreement between APL-SRI-JPL that made wafers available for this work.\n\nSubmitted - 2112.01691.pdf
", "abstract": "CMOS detectors offer many advantages over CCDs for optical and UV astronomical applications, especially in space where high radiation tolerance is required. However, astronomical instruments are most often designed for low light-level observations demanding low dark current and read noise, good linearity and high dynamic range, characteristics that have not been widely demonstrated for CMOS imagers. We report the performance, over temperatures from 140 - 240 K, of a radiation hardened SRI 4Kx2K back-side illuminated CMOS image sensor with surface treatments that make it highly sensitive in blue and UV bands. After suppressing emission from glow sites resulting from defects in the engineering grade device examined in this work, a 0.077 me\u207b/s dark current floor is reached at 160 K, rising to 1 me\u207b/s at 184 K, rivaling that of the best CCDs. We examine the trade-off between readout speed and read noise, finding that 1.43 e\u207b median read noise is achieved using line-wise digital correlated double sampling at 700 kpix/s/ch corresponding to a 1.5 s readout time. The 15 ke\u207b well capacity in high gain mode extends to 120 ke\u207b in dual gain mode. Continued collection of photo-generated charge during readout enables a further dynamic range extension beyond 10\u2076 e\u207b effective well capacity with only 1% loss of exposure efficiency by combining short and long exposures. A quadratic fit to correct for non-linearity reduces gain correction residuals from 1.5% to 0.2% in low gain mode and to 0.4% in high gain mode. Cross-talk to adjacent pixels is only 0.4% vertically, 0.6% horizontally and 0.1% diagonally. These characteristics plus the relatively large 10 \u03bcm pixel size, quasi 4-side buttability, electronic shutter and sub-array readout make this sensor an excellent choice for wide field astronomical imaging in space, even at FUV wavelengths where sky background is very low.", "date": "2021-12-03", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20220119-233946472", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220119-233946472", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL President and Director's Fund" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.2112.01691", "primary_object": { "basename": "2112.01691.pdf", "url": "https://authors.library.caltech.edu/records/p7s73-fem72/files/2112.01691.pdf" }, "pub_year": "2021", "author_list": "Greffe, Timothee; Smith, Roger; et al." }, { "id": "https://authors.library.caltech.edu/records/8ydzc-cn778", "eprint_id": 112893, "eprint_status": "archive", "datestamp": "2023-08-20 06:10:34", "lastmod": "2025-06-30 18:18:17", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bachetti-Matteo", "name": { "family": "Bachetti", "given": "Matteo" }, "orcid": "0000-0002-4576-9337" }, { "id": "Heida-Marianne", "name": { "family": "Heida", "given": "Marianne" }, "orcid": "0000-0002-1082-7496" }, { "id": "Maccarone-Thomas-J", "name": { "family": "Maccarone", "given": "Thomas" }, "orcid": "0000-0003-0976-4755" }, { "id": "Huppenkothen-Daniela", "name": { "family": "Huppenkothen", "given": "Daniela" }, "orcid": "0000-0002-1169-7486" }, { "id": "Israel-Gian-Luca", "name": { "family": "Israel", "given": "Gian Luca" } }, { "id": "Barret-Didier", "name": { "family": "Barret", "given": "Didier" }, "orcid": "0000-0002-0393-9190" }, { "id": "Brightman-Murray", "name": { "family": "Brightman", "given": "Murray" }, "orcid": "0000-0002-8147-2602" }, { "id": "Brumback-McKinley-C", "name": { "family": "Brumback", "given": "McKinley" }, "orcid": "0000-0002-4024-6967" }, { "id": "Earnshaw-Hannah-P", "name": { "family": "Earnshaw", "given": "Hannah P." }, "orcid": "0000-0001-5857-5622" }, { "id": "Forster-Karl", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "F\u00fcrst-Felix", "name": { "family": "F\u00fcrst", "given": "Felix" }, "orcid": "0000-0003-0388-0560" }, { "id": "Grefenstette-Brian-W", "name": { "family": "Grefenstette", "given": "Brian W." }, "orcid": "0000-0002-1984-2932" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0002-4226-8959" }, { "id": "Jaodand-Amruta-D", "name": { "family": "Jaodand", "given": "Amruta D." }, "orcid": "0000-0002-3850-6651" }, { "id": "Madsen-Kristin-K", "name": { "family": "Madsen", "given": "Kristin K." }, "orcid": "0000-0003-1252-4891" }, { "id": "Middleton-Matthew-J", "name": { "family": "Middleton", "given": "Matthew" }, "orcid": "0000-0002-8183-2970" }, { "id": "Pike-Sean-N", "name": { "family": "Pike", "given": "Sean N." }, "orcid": "0000-0002-8403-0041" }, { "id": "Pilia-Maura", "name": { "family": "Pilia", "given": "Maura" } }, { "id": "Poutanen-J", "name": { "family": "Poutanen", "given": "Juri" }, "orcid": "0000-0002-0983-0049" }, { "id": "Stern-Daniel", "name": { "family": "Stern", "given": "Daniel" }, "orcid": "0000-0003-2686-9241" }, { "id": "Tomsick-John-A", "name": { "family": "Tomsick", "given": "John A." }, "orcid": "0000-0001-5506-9855" }, { "id": "Walton-Dominic-J", "name": { "family": "Walton", "given": "Dominic J." }, "orcid": "0000-0001-5819-3552" }, { "id": "Webb-Natalie-A", "name": { "family": "Webb", "given": "Natalie" } }, { "id": "Wilms-J\u00f6rn", "name": { "family": "Wilms", "given": "J\u00f6rn" }, "orcid": "0000-0003-2065-5410" } ] }, "title": "The extreme mass transfer and high magnetic field of the first ultraluminous pulsar M82 X-2", "ispublished": "unpub", "full_text_status": "public", "note": "The authors wish to thank W\u0142odek Klu\u017aniak and Alessandro Ridolfi for useful discussions, and the staff at the NuSTAR Science Operations Center at Caltech for the help in scheduling the observations and the frequent clock correction file updates, that allowed a prompt analysis of the data. MB was funded in part by PRIN TEC INAF 2019 \"SpecTemPolar! \u2013 Timing analysis in the era of high-throughput photon detectors\". MH is supported by an ESO fellowship. GLI acknowledges funding from the Italian MIUR PRIN grant 2017LJ39LM. ADJ was funded in part by the Chandra grant 803-0000-716015-404H00-6100-2723-4210-40716015HH83121. JP was supported by the grant 14.W03.31.0021 of the Ministry of Science and Higher Education of the Russian Federation and the Academy of Finland grant 333112. DJW acknowledges support from STFC in the form of an Ernest Rutherford Fellowship. HPE acknowledges support under NASA Contract No. NNG08FD60C. \n\nAll the analysis of this Paper was done using open-source software: Astropy, Stingray, HENDRICS, PINT, emcee, corner, scinum, and can easily be verified using the solution in Table 1. Figures were produced using the Matplotlib library and the Veusz software. The data used for this work come from the NuSTAR mission and are usually held private for one year, and made public on the High Energy Astrophysics Science archive (HEASARC) afterwise. NuSTAR is a Small Explorer mission led by Caltech and managed by JPL for NASA's Science Mission Directorate in Washington. NuSTAR was developed in partnership with the Danish Technical University and the Italian Space Agency (ASI). The spacecraft was built by Orbital Sciences Corp., Dulles, Virginia.\n\nSubmitted - 2112.00339.pdf
", "abstract": "M82 X-2 is the first pulsating ultraluminous X-ray source (PULX) discovered. The luminosity of these extreme pulsars, if isotropic, implies an extreme mass transfer rate. An alternative is to assume a much lower mass transfer rate, but an apparent luminosity boosted by geometrical beaming. Only an independent measurement of the mass transfer can help discriminate between these two scenarios. In this Paper, we follow the orbit of the neutron star for seven years, measure the decay of the orbit, and demonstrate that this orbital decay is driven by extreme mass transfer of more than 150 times the mass transfer limit set by the Eddington luminosity. This measurement shows that the mass available to the accretor is more than enough to justify its luminosity, with no need for beaming. This also strongly favors models where the accretor is a highly-magnetized neutron star.", "date": "2021-12-01", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20220113-234521215", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220113-234521215", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "PRIN 2019" }, { "agency": "European Southern Observatory (ESO)" }, { "agency": "Ministero dell'Istruzione, dell'Universit\u00e0 e della Ricerca (MIUR)", "grant_number": "2017LJ39LM" }, { "agency": "Chandra", "grant_number": "803-0000-716015-404H00-6100-2723-4210-40716015HH83121" }, { "agency": "Ministry of Science and Higher Education of the Russian Federation", "grant_number": "14.W03.31.0021" }, { "agency": "Academy of Finland", "grant_number": "333112" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA", "grant_number": "NNG08FD60C" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "NuSTAR" }, { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.2112.00339", "primary_object": { "basename": "2112.00339.pdf", "url": "https://authors.library.caltech.edu/records/8ydzc-cn778/files/2112.00339.pdf" }, "pub_year": "2021", "author_list": "Bachetti, Matteo; Heida, Marianne; et al." }, { "id": "https://authors.library.caltech.edu/records/yqpbf-qmh66", "eprint_id": 112872, "eprint_status": "archive", "datestamp": "2023-08-20 05:41:08", "lastmod": "2025-06-30 18:18:14", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Madsen-Kristin-K", "name": { "family": "Madsen", "given": "Kristin K." }, "orcid": "0000-0003-1252-4891" }, { "id": "Forster-Karl", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Grefenstette-Brian-W", "name": { "family": "Grefenstette", "given": "Brian" }, "orcid": "0000-0002-1984-2932" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0002-4226-8959" }, { "id": "Miyasaka-Hiromasa", "name": { "family": "Miyasaka", "given": "Hiromasa" }, "orcid": "0000-0002-8074-4186" } ] }, "title": "2021 Effective Area calibration of the Nuclear Spectroscopic Telescope ARray (NuSTAR)", "ispublished": "unpub", "full_text_status": "public", "keywords": "NuSTAR, X-ray, Satellite", "note": "This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Space Science Data Center (SSDC, Italy) and the California Institute of Technology (USA). This material is based upon work supported by NASA under award number 80GSFC21M0002. We thank Murray Brightman, Renee Ludlam, Guglielmo Mastroserio, and Riley Connors for performing the case study re-analyses in \u00a77.2.\n\nSubmitted - 2110.11522.pdf
", "abstract": "We present here the updated calibration of The Nuclear Spectroscopic Telescope ARray NuSTAR, which was performed using data on the Crab accumulated over the last 9 years in orbit. The basis for this new calibration contains over 250ks of focused Crab (imaged through the optics) and over 500ks of stray-light Crab (not imaged through optics). We measured an epoch averaged Crab spectrum of the stray-light Crab data and define a canonical Crab spectrum of \u0393 = 2.103 \u00b1 0.001 and N = 9.69 \u00b1 0.02 keV\u207b\u00b9 cm\u207b\u00b2 s\u207b\u00b9 at 1 keV, which we use as our calibration standard. The new calibration, released in the CALDB update 20211020, provides significant updates to: 1) the detector absorption component, 2) the detector response function, and 3) the effective area vignetting function. The calibration improves agreement between FPMA and FPMB across detectors with a standard deviation of 1.7% for repeat observations between off-axis angles of 1-4 arcmin, and the measured flux has increased by 5-15%, with 5% below 1 arcmin off-axis angle, 10% between 1-2 arcmin, and 15 above 4arcmin.", "date": "2021-10-21", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20220113-182222694", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220113-182222694", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG08FD60C" }, { "agency": "NASA", "grant_number": "80GSFC21M0002" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "NuSTAR" } ] }, "doi": "10.48550/arXiv.2110.11522", "primary_object": { "basename": "2110.11522.pdf", "url": "https://authors.library.caltech.edu/records/yqpbf-qmh66/files/2110.11522.pdf" }, "pub_year": "2021", "author_list": "Madsen, Kristin K.; Forster, Karl; et al." }, { "id": "https://authors.library.caltech.edu/records/76db7-chf58", "eprint_id": 103720, "eprint_status": "archive", "datestamp": "2023-08-19 21:47:11", "lastmod": "2025-02-01 18:09:21", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Makhathini-S", "name": { "family": "Makhathini", "given": "Sphesihle" } }, { "id": "Mooley-Kunal-Prakash", "name": { "family": "Mooley", "given": "Kunal P." }, "orcid": "0000-0002-2557-5180" }, { "id": "Brightman-M", "name": { "family": "Brightman", "given": "Murray" }, "orcid": "0000-0002-8147-2602" }, { "name": { "family": "Hotokezaka", "given": "Kenta" }, "orcid": "0000-0002-2502-3730" }, { "name": { "family": "Nayana", "given": "A. J." } }, { "name": { "family": "Intema", "given": "Huib T." }, "orcid": "0000-0002-5880-2730" }, { "name": { "family": "Dobie", "given": "Dougal" }, "orcid": "0000-0003-0699-7019" }, { "name": { "family": "Lenc", "given": "E." }, "orcid": "0000-0002-9994-1593" }, { "name": { "family": "Perley", "given": "Daniel A." }, "orcid": "0000-0001-8472-1996" }, { "id": "Fremling-C", "name": { "family": "Fremling", "given": "Christoffer" }, "orcid": "0000-0002-4223-103X" }, { "name": { "family": "Moldon", "given": "Javier" } }, { "name": { "family": "Lazzati", "given": "Davide" }, "orcid": "0000-0002-9190-662X" }, { "name": { "family": "Kaplan", "given": "David L." }, "orcid": "0000-0001-6295-2881" }, { "name": { "family": "Balasubramanian", "given": "Arvind" } }, { "name": { "family": "Brown", "given": "Ian" } }, { "name": { "family": "Carbone", "given": "Dario" }, "orcid": "0000-0002-6575-4642" }, { "name": { "family": "Chandra", "given": "Poonam" }, "orcid": "0000-0002-0844-6563" }, { "name": { "family": "Corsi", "given": "Alessandra" } }, { "name": { "family": "Camilo", "given": "Fernando" }, "orcid": "0000-0002-1873-3718" }, { "name": { "family": "Deller", "given": "Adam T." }, "orcid": "0000-0001-9434-3837" }, { "name": { "family": "Frail", "given": "Dale A." } }, { "name": { "family": "Murphy", "given": "Tara" }, "orcid": "0000-0002-2686-438X" }, { "name": { "family": "Murphy", "given": "Eric J." }, "orcid": "0000-0001-7089-7325" }, { "name": { "family": "Nakar", "given": "Ehud" }, "orcid": "0000-0002-4534-7089" }, { "name": { "family": "Smirnov", "given": "Oleg" } }, { "name": { "family": "Beswick", "given": "Robert" } }, { "name": { "family": "Fender", "given": "Rob" } }, { "id": "Hallinan-G", "name": { "family": "Hallinan", "given": "Gregg" }, "orcid": "0000-0002-7083-4049" }, { "name": { "family": "Heywood", "given": "Ian" } }, { "id": "Kasliwal-M-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938" }, { "id": "Lee-Bomee", "name": { "family": "Lee", "given": "Bomee" }, "orcid": "0000-0003-1954-5046" }, { "id": "Lu-Wenbin", "name": { "family": "Lu", "given": "Wenbin" }, "orcid": "0000-0002-1568-7461" }, { "name": { "family": "Rana", "given": "Javed" }, "orcid": "0000-0001-5605-1809" }, { "name": { "family": "Perkins", "given": "S. J." } }, { "name": { "family": "White", "given": "Sarah V." } }, { "name": { "family": "Jozsa", "given": "Gyula I." } }, { "name": { "family": "Hugo", "given": "Benjamin" } }, { "name": { "family": "Kamphuis", "given": "Peter" } } ] }, "title": "The Panchromatic Afterglow of GW170817: The full uniform dataset, modeling, comparison with previous results and implications", "ispublished": "unpub", "full_text_status": "public", "keywords": "gravitational waves - stars: neutron - radio continuum: stars - X-rays: stars - infrared: stars", "note": "The MeerKAT telescope is operated by the South African Radio Astronomy Observatory, which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The authors thank the NRAO staff, especially Mark Claussen and Amy Mioduszewski, for scheduling the VLA observations. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. The MeerKAT telescope is operated by the South African Radio Astronomy Observatory, (SARAO), which is a facility of the National Research Foundation (NRF), an agency of the Department of Science and Technology. The authors are grateful to Schuyler van Dyk for helpful discussions. KPM is a Jansky Fellow of the National Radio Astronomy Observatory. DD is supported by an Australian Government Research Training Program Scholarship. TM acknowledges the support of the Australian Research Council through grant DP190100561. Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), project number CE170100004. We acknowledge support by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation PIRE (Partnership in International Research and Education) program under Grant No 1545949. DL acknowledges support from NASA grants 80NSSC18K1729 (Fermi) and NNX17AK42G (ATP), Chandra grant TM9-20002X, and NSF grant AST-1907955. This research has made use of NASA's Astrophysics Data System Bibliographic Services. CF gratefully acknowledges support of his research by the Heising-Simons Foundation. JM acknowledges financial support from the State Agency for Research of the Spanish MCIU through the \"Center of Excellence Severo Ochoa\" award to the Instituto de Astrof\u00edsica de Andaluc\u00eda (SEV-2017-0709) and from the grant RTI2018-096228-B-C31 (MICIU/FEDER, EU). DLK was supported by NSF grant AST-1816492 PK is partially supported by the BMBF project 05A17PC2 for D-MeerKAT. \n\nFacility: VLA, ATCA, uGMRT, MeerKAT, eMERLIN, HST, Chandra, XMM-Newton Software: MIRIAD (Sault et al. 1995), CASA (McMullin et al. 2007), emcee (Foreman-Mackey et al. 2013), corner (Foreman-Mackey 2016) , CARACal (Ramatsoku et al. 2020), AOFlagger (Offringa et al. 2010), WSClean (Offringa et al. 2014), CubiCal (Kenyon et al. 2018), MeqTrees (Noordam & Smirnov 2010)\n\nSubmitted - 2006.02382.pdf
", "abstract": "We present the full panchromatic afterglow light curve data of GW170817, including new radio data as well as archival optical and X-ray data, between 0.5 and 940 days post-merger. By compiling all archival data, and reprocessing a subset of it, we have ensured that the panchromatic dataset is uniform and therefore immune to the differences in data processing or flux determination methods used by different groups. Simple power-law fits to the uniform afterglow light curve indicate a t^(0.86\u00b10.04) rise, a t^(\u22121.90\u00b10.12) decline, and a peak occurring at 155\u00b14 days. The afterglow is optically thin throughout its evolution, consistent with a single spectral index (\u22120.569\u00b10.002) across all epochs. This gives a precise and updated estimate of the electron power-law index, p=2.138\u00b10.004. By studying the diffuse X-ray emission from the host galaxy, we place a conservative upper limit on the hot ionized ISM density, <0.01 cm\u207b\u00b3, consistent with previous afterglow studies. Using the late-time afterglow data we rule out any long-lived neutron star remnant having magnetic field strength between 10^(10.4) G and 10\u00b9\u2076 G. Our fits to the afterglow data using an analytical model that includes VLBI proper motion from Mooley et al (2018), and a structured jet model that ignores the proper motion, indicates that the proper motion measurement needs to be considered while seeking an accurate estimate of the viewing angle.", "date": "2020-06-03", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200604-151511891", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151511891", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Research Foundation (South Africa)" }, { "agency": "Department of Science and Innovation (South Africa)" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "Commonwealth Scientific and Industrial Research Organisation (CSIRO)" }, { "agency": "Tata Institute of Fundamental Research" }, { "agency": "South African Radio Astronomy Observatory (SARAO)" }, { "agency": "Jansky Fellowship" }, { "agency": "Australian Research Council", "grant_number": "DP190100561" }, { "agency": "Australian Research Council", "grant_number": "CE170100004" }, { "agency": "NSF", "grant_number": "AST-1545949" }, { "agency": "NASA", "grant_number": "80NSSC18K1729" }, { "agency": "NASA", "grant_number": "NNX17AK42G" }, { "agency": "NASA", "grant_number": "TM9-20002X" }, { "agency": "NSF", "grant_number": "AST-1907955" }, { "agency": "Heising-Simons Foundation" }, { "agency": "Severo Ochoa", "grant_number": "SEV-2017-0709" }, { "agency": "Ministerio de Ciencia, Innovaci\u00f3n y Universidades (MICIU)", "grant_number": "RTI2018-096228-B-C31" }, { "agency": "Fondo Europeo de Desarrollo Regional (FEDER)" }, { "agency": "NSF", "grant_number": "AST-1816492" }, { "agency": "Bundesministerium f\u00fcr Bildung und Forschung (BMBF)", "grant_number": "05A17PC2" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Space-Radiation-Laboratory" }, { "id": "NuSTAR" } ] }, "doi": "10.48550/arXiv.2006.02382", "primary_object": { "basename": "2006.02382.pdf", "url": "https://authors.library.caltech.edu/records/76db7-chf58/files/2006.02382.pdf" }, "pub_year": "2020", "author_list": "Makhathini, Sphesihle; Mooley, Kunal P.; et al." }, { "id": "https://authors.library.caltech.edu/records/v2mas-3we29", "eprint_id": 103715, "eprint_status": "archive", "datestamp": "2023-08-19 21:20:56", "lastmod": "2025-06-30 18:32:54", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Madsen-K-K", "name": { "family": "Madsen", "given": "Kristin K." }, "orcid": "0000-0003-1252-4891" }, { "id": "Grefenstette-B-W", "name": { "family": "Grefenstette", "given": "Brian W." }, "orcid": "0000-0002-1984-2932" }, { "id": "Pike-S-N", "name": { "family": "Pike", "given": "Sean" }, "orcid": "0000-0002-8403-0041" }, { "id": "Miyasaka-Hiromasa", "name": { "family": "Miyasaka", "given": "Hiromasa" }, "orcid": "0000-0002-8074-4186" }, { "id": "Brightman-M", "name": { "family": "Brightman", "given": "Murray" }, "orcid": "0000-0002-8147-2602" }, { "id": "Forster-K", "name": { "family": "Forster", "given": "Karl" }, "orcid": "0000-0001-5800-5531" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0002-4226-8959" } ] }, "title": "NuSTAR low energy effective area correction due to thermal blanket tear", "ispublished": "unpub", "full_text_status": "public", "keywords": "space vehicles: instruments", "note": "This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). \n\nFacility: NuSTAR\n\nThis document serves as a technical note for the NuSTAR CALDB version 20200429. The CADLB release is the first in a two parts made to address the problem described in the paper. The paper will be updated with the second release, and will be submitted to a journal after the final release.\n\nSubmitted - 2005.00569.pdf
", "abstract": "A rip in the MLI at the exit aperture of OMA, the NuSTAR optic aligned with detector focal plane module FPMA, has resulted in an increased photon flux through OMA that has manifested itself as a low energy excess. Overall, the MLI coverage has decreased by 10%, but there is an additional time-varying component, which occasionally causes the opening to increase by up to 20%. We address the problem with a calibration update, and in this paper, we describe the attributes of the problem, the implications it has on data analysis, and the solution.", "date": "2020-05-01", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200604-151455025", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151455025", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG08FD60C" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Space-Radiation-Laboratory" }, { "id": "NuSTAR" } ] }, "doi": "10.48550/arXiv.2005.00569", "primary_object": { "basename": "2005.00569.pdf", "url": "https://authors.library.caltech.edu/records/v2mas-3we29/files/2005.00569.pdf" }, "pub_year": "2020", "author_list": "Madsen, Kristin K.; Grefenstette, Brian W.; et al." }, { "id": "https://authors.library.caltech.edu/records/759r9-q6z09", "eprint_id": 100345, "eprint_status": "archive", "datestamp": "2023-08-19 15:30:36", "lastmod": "2025-02-01 17:13:41", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "O'Sullivan-Donal", "name": { "family": "O'Sullivan", "given": "Donal" }, "orcid": "0000-0002-4959-9179" }, { "id": "Matuszweski-M", "name": { "family": "Matuszweski", "given": "Mateusz" } }, { "id": "Hamden-E-T", "name": { "family": "Hamden", "given": "Erika" }, "orcid": "0000-0002-3131-7372" }, { "id": "Dekel-A", "name": { "family": "Dekel", "given": "Avishai" }, "orcid": "0000-0003-4174-0374" }, { "id": "Lapiner-Sharon", "name": { "family": "Lapiner", "given": "Sharon" } }, { "id": "Morrissey-P", "name": { "family": "Morrissey", "given": "Patrick" }, "orcid": "0000-0001-8177-1023" }, { "id": "Neill-J-D", "name": { "family": "Neill", "given": "James D." }, "orcid": "0000-0002-0466-1119" }, { "id": "Cantalupo-S", "name": { "family": "Cantalupo", "given": "Sebastiano" }, "orcid": "0000-0001-5804-1428" }, { "id": "Prochaska-J-X", "name": { "family": "Prochaska", "given": "J. Xavier" }, "orcid": "0000-0002-7738-6875" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles" }, "orcid": "0000-0002-4834-7260" }, { "id": "Trainor-R-F", "name": { "family": "Trainor", "given": "Ryan" }, "orcid": "0000-0002-6967-7322" }, { "id": "Moore-A-M", "name": { "family": "Moore", "given": "Anna" }, "orcid": "0000-0002-2894-6936" }, { "id": "Ceverino-D", "name": { "family": "Ceverino", "given": "Daniel" }, "orcid": "0000-0002-8680-248X" }, { "id": "Primack-J-R", "name": { "family": "Primack", "given": "Joel" }, "orcid": "0000-0001-5091-5098" }, { "id": "Rizzi-L", "name": { "family": "Rizzi", "given": "Luca" }, "orcid": "0000-0003-0882-2327" } ] }, "title": "Multi-Filament Inflows Fueling Young Star Forming Galaxies", "ispublished": "unpub", "full_text_status": "public", "note": "This work was supported by the National Science Foundation, the W. M Keck Observatory and the California Institute of Technology. The VELA simulations were performed at NASA Advanced Supercomputing (NAS) at NASA Ames Research Center. D.C. is funded by the ERC Advanced Grant, STARLIGHT: Formation of the First Stars (project number 339177). \n\nAuthor Contributions: D.C.M. is the Principal Investigator of KCWI, performed the analysis of the simulated galaxy, data and MFI models, and was principal author on the paper. D.O. and D.C.M led the observations of UM287 and CSO 38. D.O., M.M. reduced the data. D. O., M. M., and E. H. contributed to the paper writing. P.M., M.M., D.C.M., D.N., D.O., and A.M. designed, constructed, and operated KCWI. D.N., M.M. and D.C.M. developed the KCWI data pipeline and produced the final data cubes. D. C. developed the VELA simulations. A.D. and S. L. provided the simulated galaxy VELA07 and contributed to the paper. D.C. and J.P. contributed the cosmological simulation. C.S, R.T., S.C., and J.X.P. contributed to the development of KCWI, Keck data for the two protogalaxies, and to the editing of the paper. L. R. made major contributions to KCWI commissioning and participated in the observations of CSO 38. \n\nCode and Data Availability: KCWI pipeline code is available on the W. M. Keck Observatory website. KCWI data on CSO38 and UM287 is publically available. Data on UM287 will be available 18 months after the observation in Oct 2017. The data that support the plots within this paper and other findings of this study are available from the corresponding author upon reasonable request.\n\nSubmitted - 1904.11465.pdf
", "abstract": "Theory suggests that there are two primary modes of accretion through which dark matter halos acquire the gas to form and fuel galaxies, hot and cold mode accretion. In cold mode accretion, gas streams along cosmic web filaments to the center of the halo, allowing for the efficient delivery of star-forming fuel. Recently, two QSO-illuminated HI Lyman alpha (Ly{\\alpha}) emitting objects were reported to have properties of cold, rotating structures (Martin et al. 2015, Martin et al. 2016). However, the spatial and spectral resolution available was insufficient to constrain radial flows associated with connecting filaments. With the Keck Cosmic Web Imager (KCWI) we now have eight times the spatial resolution, permitting the detection of these in-spiraling flows. In order to detect these inflows, we introduce a suite of models which incorporate zonal radial flows, demonstrate their performance on a numerical simulation that exhibits coldflow accretion, and show that they are an excellent match to KCWI velocity maps of two Ly{\\alpha} emitters observed around high-redshift quasars. These Multi-Filament Inflow models kinematically isolate zones of radial inflow that correspond to extended filamentary emission. The derived gas flux and inflow path is sufficient to fuel the inferred central galaxy star formation rate and angular momentum. Thus, our kinematic emission maps provide strong evidence for the inflow of gas from the cosmic web building galaxies at the peak of star formation.", "date": "2019-04-25", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20191218-101527501", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191218-101527501", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "W. M. Keck Observatory" }, { "agency": "Caltech" }, { "agency": "European Research Council (ERC)", "grant_number": "339177" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Astronomy-Department" } ] }, "doi": "10.48550/arXiv.1904.11465", "primary_object": { "basename": "1904.11465.pdf", "url": "https://authors.library.caltech.edu/records/759r9-q6z09/files/1904.11465.pdf" }, "pub_year": "2019", "author_list": "Martin, D. Christopher; O'Sullivan, Donal; et al." }, { "id": "https://authors.library.caltech.edu/records/5me0w-mkc17", "eprint_id": 101100, "eprint_status": "archive", "datestamp": "2023-09-15 06:26:27", "lastmod": "2025-02-02 04:03:41", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Webber-W-R", "name": { "family": "Webber", "given": "W. R." } }, { "id": "Lal-Nand", "name": { "family": "Lal", "given": "N." } }, { "id": "Stone-E-C", "name": { "family": "Stone", "given": "E. C." }, "orcid": "0000-0002-2010-5462" }, { "id": "Cummings-A-C", "name": { "family": "Cummings", "given": "A. C." }, "orcid": "0000-0002-3840-7696" }, { "id": "Heikkila-B-C", "name": { "family": "Heikkila", "given": "B." } } ] }, "title": "Voyager 1 Measurements Beyond the Heliopause of Galactic Cosmic Ray Helium, Boron, Carbon, Oxygen, Magnesium, Silicon and Iron Nuclei with Energies 0.5 to >1.5 GeV/nuc", "ispublished": "unpub", "full_text_status": "public", "note": "The authors are grateful to the Voyager team that designed and built the CRS experiment with the hope that one day it would measure the galactic spectra of nuclei and electrons. This includes the present team with Ed Stone as PI, Alan Cummings, Nand Lal and Bryant Heikkila, and to others who are no longer members of the team, F.B. McDonald and R.E. Vogt. Their prescience will not be forgotten. This work has been supported by NASA Grant NNN12AA01C.\n\nSubmitted - 1712.02818.pdf
", "abstract": "We have obtained the energy spectra of cosmic ray He, B, C, O, Mg, S and Fe nuclei in the range 0.5-1.5 GeV/nuc and above using the penetrating particle mode of the High Energy Telescope, part of the Cosmic Ray Science (CRS) experiment on Voyagers 1 and 2. The data analysis procedures are the same as those used to obtain similar spectra from the identical V2 HET telescope while it was in the heliosphere between about 23 and 54 AU. The time period of analysis includes 4 years of data beyond the heliopause (HP). These new interstellar spectra are compared with various earlier experiments at the same energies at the Earth to determine the solar modulation parameter, \u03a6. These new spectra are also compared with recent measurements of the spectra of the same nuclei measured by the same telescope at low energies. It is found that the ratio of intensities at 100 MeV/nuc to those at 1.0 GeV/nuc are significantly Z dependent. Some of this Z dependence can be explained by the Z\u00b2 dependence of energy loss by ionization in the 7-10 g/cm\u00b2 of interstellar H and He traversed by cosmic rays of these energies in the galaxy; some by the Z dependent loss due to nuclear interactions in this same material; some by possible differences in the source spectra of these nuclei and some by the non-uniformity of the source distribution and propagation conditions. The observed features of the spectra, also including a Z dependence of the peak intensities of the various nuclei, pose interesting problems related to the propagation and source distribution of these cosmic rays.", "date": "2017-12-07", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200204-081707376", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-081707376", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNN12AA01C" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.1712.02818", "primary_object": { "basename": "1712.02818.pdf", "url": "https://authors.library.caltech.edu/records/5me0w-mkc17/files/1712.02818.pdf" }, "pub_year": "2017", "author_list": "Webber, W. R.; Lal, N.; et al." }, { "id": "https://authors.library.caltech.edu/records/0a850-j0f82", "eprint_id": 101101, "eprint_status": "archive", "datestamp": "2023-08-19 03:37:20", "lastmod": "2025-02-01 17:16:10", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Webber-W-R", "name": { "family": "Webber", "given": "W. R." } }, { "id": "Stone-E-C", "name": { "family": "Stone", "given": "E. C." }, "orcid": "0000-0002-2010-5462" }, { "id": "Cummings-A-C", "name": { "family": "Cummings", "given": "A. C." }, "orcid": "0000-0002-3840-7696" }, { "id": "Heikkila-B-C", "name": { "family": "Heikkila", "given": "B." } }, { "id": "Lal-Nand", "name": { "family": "Lal", "given": "N." } } ] }, "title": "The Intensities of Cosmic Ray H and He Nuclei at ~250 MeV/nuc Measured by Voyagers 1 and 2 - Using these Intensities to Determine the Solar Modulation Parameter in the Inner Heliosphere and the Heliosheath Over a 40 Year Time Period", "ispublished": "unpub", "full_text_status": "public", "note": "The authors wish to thank JPL for their unfailing support, both moral and financial, for 40 years since the launch of V1 and V2 in August, 1977.\n\nSubmitted - 1706.02772.pdf
", "abstract": "We have determined the solar modulation potential, \u03a6, vs. time that is observed at Voyager 1 and 2 from measurements of the H and He nuclei intensities at a common energy of 250 MeVnuc. The H nuclei have a rigidity 0.7 GV, the He nuclei 1.4 GV. These measurements cover a 40 year time period, which includes almost 4 cycles of solar 11 year sunspot variations, throughout the inner heliosphere out to the HTS at distances of 95 AU and 85 AU, respectively at V1 and V2, and then beyond in the heliosheath. Inside the HTS the modulation potential vs. time curves at V1 and V2 show a very similar temporal structure to those observed at the Earth. During a later period of maximum solar modulation from 2000.0 to 2005.0 when V1 and V2 are in the outer heliosphere between 60-94 AU, the main temporal features of the modulation potential curves at all 3 locations match up with appropriate time delays at V1 and V2 if it is assumed that spatially coherent structures are moving outward past V1 and V2, with outward speeds of up to 700 Kms\u207b\u00b9. After 2004.0 V1 and V2 are at latitudes of +35\u00b0 and -30\u00b0 respectively, placing lower limits on the latitude extent of these structures. Beyond the HTS in the heliosheath the modulation potential slowly decreases at both spacecraft with only a weak evidence of the unusual modulation minimum observed at the Earth in 2009, for example. A sudden decrease of the modulation potential 50 MV for both H and He nuclei occurs at V1 just before the heliopause crossing at about 122 AU. This decrease has not yet been observed at V2, which is now at 113 AU and still observing a modulation potential 60 MV.", "date": "2017-06-08", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200204-082135453", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-082135453", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.1706.02772", "primary_object": { "basename": "1706.02772.pdf", "url": "https://authors.library.caltech.edu/records/0a850-j0f82/files/1706.02772.pdf" }, "pub_year": "2017", "author_list": "Webber, W. R.; Stone, E. C.; et al." }, { "id": "https://authors.library.caltech.edu/records/xrp58-d7449", "eprint_id": 101103, "eprint_status": "archive", "datestamp": "2023-08-19 13:47:23", "lastmod": "2025-02-01 17:16:13", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Webber-W-R", "name": { "family": "Webber", "given": "W. R." } }, { "id": "McDonald-F-B", "name": { "family": "McDonald", "given": "F. B." } }, { "id": "Cummings-A-C", "name": { "family": "Cummings", "given": "A. C." }, "orcid": "0000-0002-3840-7696" }, { "id": "Stone-E-C", "name": { "family": "Stone", "given": "E. C." }, "orcid": "0000-0002-2010-5462" }, { "id": "Heikkila-B-C", "name": { "family": "Heikkila", "given": "B." } }, { "id": "Lal-Nand", "name": { "family": "Lal", "given": "N." } } ] }, "title": "At Voyager 1 Starting on about August 25, 2012 at a Distance of 121.7 AU From the Sun, a Sudden Disappearance of Anomalous Cosmic Rays and an Unusually Large Sudden Increase of Galactic Cosmic Ray H and He Nuclei and Electron Occurred", "ispublished": "unpub", "full_text_status": "public", "note": "This article was conceived by our Voyager colleague, Frank McDonald, who is no longer with us. Frank, we have been working together for over 55 years to reach the goal of actually observing the interstellar spectra of cosmic rays, possibly now achieved almost on the day of your passing. You wanted so badly to finish this article that you had already started. Together we did it. Bon Voyage!\n\nSubmitted - 1212.0883.pdf
", "abstract": "At the Voyager 1 spacecraft in the outer heliosphere, after a series of complex intensity changes starting at about May 8th, the intensities of both anomalous cosmic rays (ACR) and galactic cosmic rays (GCR) changed suddenly and decisively on August 25th (121.7 AU from the Sun). The ACR started the intensity decrease with an initial e-folding rate of intensity decrease of ~1 day. Within a matter of a few days, the intensity of 1.9-2.7 MeV protons and helium nuclei had decreased to less than 0.1 of their previous value and after a few weeks, corresponding to the outward movement of V1 by ~0.1 AU, these intensities had decreased by factors of at least 300-500 and are now lower than most estimates of the GCR spectrum for these lower energies and also at higher energies. The decrease was accompanied by large rigidity dependent anisotropies in addition to the extraordinary rapidity of the intensity changes. Also on August 25th the GCR protons, helium and heavier nuclei as well as electrons increased suddenly with the intensities of electrons reaching levels ~30-50% higher than observed just one day earlier. This increase for GCR occurred over ~1 day for the lowest rigidity electrons, and several days for the higher rigidity nuclei of rigidity ~0.5-1.0 GV. After reaching these higher levels the intensities of the GCR of all energies from 2 to 400 MeV have remained essentially constant with intensity levels and spectra that may represent the local GCR. These intensity changes will be presented in more detail in this, and future articles, as this story unfolds.", "date": "2012-12-04", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200204-084404748", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-084404748", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.1212.0883", "primary_object": { "basename": "1212.0883.pdf", "url": "https://authors.library.caltech.edu/records/xrp58-d7449/files/1212.0883.pdf" }, "pub_year": "2012", "author_list": "Webber, W. R.; McDonald, F. B.; et al." }, { "id": "https://authors.library.caltech.edu/records/v2q0q-thh59", "eprint_id": 101106, "eprint_status": "archive", "datestamp": "2023-09-15 06:26:34", "lastmod": "2025-02-02 04:03:43", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Webber-W-R", "name": { "family": "Webber", "given": "W. R." } }, { "id": "Cummings-A-C", "name": { "family": "Cummings", "given": "A. C." }, "orcid": "0000-0002-3840-7696" }, { "id": "Stone-E-C", "name": { "family": "Stone", "given": "E. C." }, "orcid": "0000-0002-2010-5462" }, { "id": "McDonald-F-B", "name": { "family": "McDonald", "given": "F. B." } }, { "id": "Intriligator-D-S", "name": { "family": "Intriligator", "given": "D. S." } }, { "id": "Higbie-P-R", "name": { "family": "Higbie", "given": "P. R." } }, { "id": "Heikkila-B-C", "name": { "family": "Heikkila", "given": "B." } }, { "id": "Lal-Nand", "name": { "family": "Lal", "given": "N." } } ] }, "title": "Large periodic time variations of termination shock particles between ~0.5-20 mev and 6-14 mev electrons measured by the crs experiment on Voyager 2 as it crossed into the heliosheath in 2007: An example of freshly accelerated cosmic rays?", "ispublished": "unpub", "full_text_status": "public", "note": "The authors all appreciate the support of the Voyager program by JPL. The data used here comes mainly from internally generated data bases which may be accessed via e-mail through the web-site (http://voyager.gsfc.nasa.gov).\n\nSubmitted - 1208.2982.pdf
", "abstract": "We have examined features in the structure of the heliosheath using the fine scale time variations of termination shock particles (TSP) between ~0.5 - 20 MeV and electrons between 2.5-14 MeV measured by the CRS instrument as the V2 spacecraft crossed the heliospheric termination shock in 2007. The very disturbed heliosheath at V2 is particularly noteworthy for strong periodic intensity variations of the TSP just after V2 crossed the termination shock (2007.66) reaching a maximum between 2007.75 and 2008.0. A series of 42/21 day periodicities was observed at V2 along with spectral changes of low energy TSP and the acceleration of 6-14 MeV electrons. Evidence is presented for the acceleration of TSP and electrons at the times of the 42/21 day periodicities just after V2 crossed the HTS. Spectra for TSP between 2-20 MeV and electrons between 2.5-14 MeV are derived for three time periods including the time of the HTS crossing. The energy spectra of TSP and electrons at these times of intensity peaks are very similar above ~3 MeV, with exponents of a power law spectrum between -3.0 and -3.6. The ratio of TSP intensities to electron intensities at the same energy is ~500. The electron intensity peaks and minima are generally out of phase with those of nuclei by ~1/2 of a 42 day cycle. These charge dependent intensity differences and the large periodic intensity changes could provide new clues as to a possible acceleration mechanism.", "date": "2012-08-14", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200204-090030437", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-090030437", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.1208.2982", "primary_object": { "basename": "1208.2982.pdf", "url": "https://authors.library.caltech.edu/records/v2q0q-thh59/files/1208.2982.pdf" }, "pub_year": "2012", "author_list": "Webber, W. R.; Cummings, A. C.; et al." }, { "id": "https://authors.library.caltech.edu/records/2j69t-cex68", "eprint_id": 101110, "eprint_status": "archive", "datestamp": "2023-08-19 09:55:02", "lastmod": "2025-02-01 17:16:15", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Webber-W-R", "name": { "family": "Webber", "given": "W. R." } }, { "id": "Cummings-A-C", "name": { "family": "Cummings", "given": "A. C." }, "orcid": "0000-0002-3840-7696" }, { "id": "Stone-E-C", "name": { "family": "Stone", "given": "E. C." }, "orcid": "0000-0002-2010-5462" }, { "id": "McDonald-F-B", "name": { "family": "McDonald", "given": "F. B." } }, { "id": "Mewaldt-R-A", "name": { "family": "Mewaldt", "given": "R. A." }, "orcid": "0000-0003-2178-9111" }, { "id": "Leske-R-A", "name": { "family": "Leske", "given": "R." }, "orcid": "0000-0002-0156-2414" }, { "id": "Wiedenbeck-M-E", "name": { "family": "Wiedenbeck", "given": "M." }, "orcid": "0000-0002-2825-3128" }, { "id": "Higbie-P-R", "name": { "family": "Higbie", "given": "P. R." } }, { "id": "Heikkila-B-C", "name": { "family": "Heikkila", "given": "B." } } ] }, "title": "20-125 MeV/nuc cosmic ray carbon nuclei intensities between 2004-2010 in solar cycle #23 as measured near the earth, at voyager 2 and also in the heliosheath at voyager 1 - modulation in a two zone heliospehre", "ispublished": "unpub", "full_text_status": "public", "note": "The authors wish to thank the Voyager team (E.C. Stone, P.I.) and the ACE team (Andrew Davis) for making their data available on their web-sites, http://voyager.gsfc.nasa.gov and http://www.srl.caltech.edu/ACE/.\n\nSubmitted - 1202.2081.pdf
", "abstract": "The recovery of cosmic ray Carbon nuclei of energy ~20-125 MeV/nuc in solar cycle #23 from 2004 to 2010 has been followed at three locations, near the Earth using ACE data and at V2 between 74-92 AU and also at V1 beyond the heliospheric termination shock at between 91-113 AU. To describe the observed intensity changes and to predict the absolute intensities measured at all three locations we have used a simple spherically symmetric (no drift) two-zone heliospheric transport model with specific values for the diffusion coefficient in both the inner and outer zones. The diffusion coefficient in the outer zone is determined to be ~5-10 times smaller than that in the inner zone out to 90 AU. For both V1 and V2 the calculated C nuclei intensities agree within an average of \u00b110% with the observed intensities. Because of this agreement between V1 and V2 observations and predictions there is no need to invoke an asymmetrical squashed heliosphere or other effects to explain the V2 intensities relative to V1 as is the case for He nuclei. The combination of the diffusion parameters used in this model and the interstellar spectrum give an unusually low overall solar modulation parameter \u03a6 = 250 MV to describe the Carbon intensities observed at the Earth in 2009. At all times both the observed and calculated spectra are very closely ~ E^(1.0) as would be expected in the adiabatic energy loss regime of solar modulation.", "date": "2012-02-09", "date_type": "published", "publisher": "arXiv", "id_number": "CaltechAUTHORS:20200204-101907790", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200204-101907790", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.1202.2081", "primary_object": { "basename": "1202.2081.pdf", "url": "https://authors.library.caltech.edu/records/2j69t-cex68/files/1202.2081.pdf" }, "pub_year": "2012", "author_list": "Webber, W. R.; Cummings, A. C.; et al." }, { "id": "https://authors.library.caltech.edu/records/yz4my-dpj75", "eprint_id": 97882, "eprint_status": "archive", "datestamp": "2023-08-19 10:54:00", "lastmod": "2025-06-30 18:32:51", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "S. R." }, "orcid": "0000-0001-5390-8563" }, { "id": "Frail-D-A", "name": { "family": "Frail", "given": "D. A." } }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "F. A." }, "orcid": "0000-0002-4226-8959" }, { "id": "Bloom-J-S", "name": { "family": "Bloom", "given": "J. S." }, "orcid": "0000-0002-7777-216X" }, { "id": "Berger-Edo", "name": { "family": "Berger", "given": "E." }, "orcid": "0000-0002-9392-9681" }, { "id": "Price-P-A", "name": { "family": "Price", "given": "P. A." } }, { "id": "Fox-D-B", "name": { "family": "Fox", "given": "D." }, "orcid": "0000-0002-3714-672X" }, { "id": "Soderberg-A-M", "name": { "family": "Soderberg", "given": "A. M." } }, { "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656" }, { "id": "Yost-S-A", "name": { "family": "Yost", "given": "S." } }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A. A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Castro-S-M", "name": { "family": "Castro", "given": "S. M." } }, { "id": "Goodrich-R-W", "name": { "family": "Goodrich", "given": "R." } }, { "id": "Chaffee-F-H", "name": { "family": "Chaffee", "given": "F." } } ] }, "title": "Cosmological Uses of Gamma-Ray Bursts", "ispublished": "unpub", "full_text_status": "public", "note": "We wish to thank numerous collaborators, and the staff of Palomar and W.M. Keck Observatories for their expert help during our observing runs. Our work was supported by grants from the NSF, NASA, and private donors.\n\nSubmitted - 0302004.pdf
", "abstract": "Studies of the cosmic gamma-ray bursts (GRBs) and their host galaxies are starting to provide interesting or even unique new insights in observational cosmology. GRBs represent a new way of identifying a population of star-forming galaxies at cosmological redshifts. GRB hosts are broadly similar to the normal field galaxy populations at comparable redshifts and magnitudes, and indicate at most a mild luminosity evolution out to z ~ 1.5 - 2. GRB optical afterglows seen in absorption provide a powerful new probe of the ISM in dense, central regions of their host galaxies, complementary to the traditional studies using QSO absorbers. Some GRB hosts are heavily obscured, and provide a new way to select a population of cosmological sub-mm sources, and a novel constraint on the total obscured fraction of star formation over the history of the universe. Finally, detection of GRB afterglows at z > 6 may provide a unique way to probe the primordial star formation, massive IMF, early IGM, and chemical enrichment at the end of the cosmic reionization era.", "date": "2003-01-31", "date_type": "published", "id_number": "CaltechAUTHORS:20190814-095417789", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190814-095417789", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" }, { "id": "Division-of-Geological-and-Planetary-Sciences" } ] }, "doi": "10.48550/arXiv.0302004", "primary_object": { "basename": "0302004.pdf", "url": "https://authors.library.caltech.edu/records/yz4my-dpj75/files/0302004.pdf" }, "pub_year": "2003", "author_list": "Djorgovski, S. G.; Kulkarni, S. R.; et al." }, { "id": "https://authors.library.caltech.edu/records/zqdjm-ha232", "eprint_id": 97661, "eprint_status": "archive", "datestamp": "2023-08-19 08:09:50", "lastmod": "2025-02-01 17:04:44", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brunner-R-J", "name": { "family": "Brunner", "given": "Robert J." } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. George" }, "orcid": "0000-0002-0603-3087" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Szalay-A-S", "name": { "family": "Szalay", "given": "Alex S." } } ] }, "title": "The National Virtual Observatory", "ispublished": "unpub", "full_text_status": "public", "note": "We are grateful to all of our collaborators from around the world who share our vision. In addition, we wish to thank NASA and NSF for their encouragement in difficult times, and both SUN Microsystems and Microsoft Research for their support. RJB would like to explicitly acknowledge financial support from NASA grants NAG5-10885 and NAG5-9482.\n\nSubmitted - 0108381.pdf
", "abstract": "As a scientific discipline, Astronomy is rather unique. We only have one laboratory, the Universe, and we cannot, of course, change the initial conditions and study the resulting effects. On top of this, acquiring Astronomical data has historically been a very labor-intensive effort. As a result, data has traditionally been preserved for posterity. With recent technological advances, however, the rate at which we acquire new data has grown exponentially, which has generated a Data Tsunami, whose wave train threatens to overwhelm the field. In this conference proceedings, we present and define the concept of virtual observatories, which we feel is the only logical answer to this dilemma.", "date": "2001-08-23", "date_type": "published", "id_number": "CaltechAUTHORS:20190805-144922867", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190805-144922867", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-10885" }, { "agency": "NASA", "grant_number": "NAG5-9482" }, { "agency": "NSF" }, { "agency": "Sun Microsystems, Inc." }, { "agency": "Microsoft Research" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "doi": "10.48550/arXiv.0108381", "primary_object": { "basename": "0108381.pdf", "url": "https://authors.library.caltech.edu/records/zqdjm-ha232/files/0108381.pdf" }, "pub_year": "2001", "author_list": "Brunner, Robert J.; Djorgovski, S. George; et al." }, { "id": "https://authors.library.caltech.edu/records/ddqjg-yba83", "eprint_id": 28196, "eprint_status": "archive", "datestamp": "2023-09-14 22:44:56", "lastmod": "2025-01-30 18:52:38", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Deelman-E", "name": { "family": "Deelman", "given": "Ewa" } }, { "id": "Kesselman-C", "name": { "family": "Kesselman", "given": "Carl" } }, { "id": "Williams-R", "name": { "family": "Williams", "given": "Roy" } }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "Albert" } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Romano-J", "name": { "family": "Romano", "given": "Joe" } }, { "id": "Allen-Bruce", "name": { "family": "Allen", "given": "Bruce" } } ] }, "title": "A Virtual Data Grid for LIGO", "ispublished": "unpub", "full_text_status": "public", "note": "Submitted - griphyn_ligo.pdf
", "abstract": "GriPhyN (Grid Physics Network) is a large US collaboration to\nbuild grid services for large physics experiments, one of which is LIGO, a\ngravitational-wave observatory. This paper explains the physics and computing\nchallenges of LIGO, and the tools that GriPhyN will build to address\nthem. A key component needed to implement the data pipeline is a virtual\ndata service; a system to dynamically create data products requested during\nthe various stages. The data could possibly be already processed in a certain\nway, it may be in a file on a storage system, it may be cached, or it may need\nto be created through computation. The full elaboration of this system will al-low\ncomplex data pipelines to be set up as virtual data objects, with existing\ndata being transformed in diverse ways.", "date": "2001", "date_type": "published", "publisher": "Lecture Notes in Computer Science", "pagerange": "3-12", "id_number": "CaltechCACR:2001.192", "isbn": "978-3-540-42293-8", "book_title": "High-Performance Computing and Networking", "official_url": "https://resolver.caltech.edu/CaltechCACR:2001.192", "rights": "You are granted permission for individual, educational, research and non-commercial reproduction, distribution, display and performance of this work in any format.", "local_group": { "items": [ { "id": "Center-for-Advanced-Computing-Research" }, { "id": "Space-Radiation-Laboratory" } ] }, "contributors": { "items": [ { "id": "Hertzberger-B", "name": { "family": "Hertzberger", "given": "Bob" } }, { "id": "Hoekstra-A", "name": { "family": "Hoekstra", "given": "Alfons" } }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "Roy" } } ] }, "primary_object": { "basename": "griphyn_ligo.pdf", "url": "https://authors.library.caltech.edu/records/ddqjg-yba83/files/griphyn_ligo.pdf" }, "pub_year": "2001", "author_list": "Deelman, Ewa; Kesselman, Carl; et al." }, { "id": "https://authors.library.caltech.edu/records/1gpae-90w41", "eprint_id": 54964, "eprint_status": "archive", "datestamp": "2023-08-19 05:47:23", "lastmod": "2025-01-30 23:31:55", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bildsten-Lars", "name": { "family": "Bildsten", "given": "Lars" }, "orcid": "0000-0001-8038-6836" }, { "id": "Rutledge-Robert-E", "name": { "family": "Rutledge", "given": "Robert E." } } ] }, "title": "Transient Low-Mass X-Ray Binaries in Quiescence", "ispublished": "unpub", "full_text_status": "public", "note": "We thank Ed Brown, George Pavlov and Slava Zavlin for the collaboration on much of this work.We are grateful to Ed Brown for preparing Fig. 3. This work was supported in part by the National Science Foundation through Grant NSF94-0174 and NASA via grant NAG5-3239. L.B. is a Cottrell Scholar of the Research Corporation.\n\nAccepted Version - 0005364.pdf
", "abstract": "We summarize the quiescent X-ray observations of transient low-mass X-ray binaries. These observations show that, in quiescence, binaries containing black holes are fainter than those containing neutron stars. This has triggered a number of theoretical ideas about what causes the quiescent X-ray emission. For black hole binaries, the options are accretion onto the black hole or coronal emission from the rapidly rotating stellar companion. There are more possibilities for the neutron stars: accretion, thermal emission from the surface or non-thermal emission from a \"turned-on\" radio pulsar. We review recent theoretical work on these mechanisms and note where current observations can distinguish between them. We highlight the re-analysis of the quiescent neutron star emission by Rutledge and collaborators that showed thermal emission to be a predominant contributor in many of these systems. Our knowledge of these binaries is bound to dramatically improve now that the Chandra and XMM satellites are operating successfully.", "date": "2000-05-17", "date_type": "published", "publisher": "????", "id_number": "CaltechAUTHORS:20150218-155519302", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150218-155519302", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 94-0174" }, { "agency": "NASA", "grant_number": "NAG5-3239" }, { "agency": "Cottrell Scholar of Research Corporation" } ] }, "other_numbering_system": { "items": [ { "id": "2000-03", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "contributors": { "items": [ { "id": "Kouveliotou-Chryssa", "name": { "family": "Kouveliotou", "given": "Chryssa" }, "orcid": "0000-0003-1443-593X" }, { "id": "Ventura-Joseph", "name": { "family": "Ventura", "given": "Joseph" } }, { "id": "Van-den-Heuvel-Ed", "name": { "family": "Van den Heuvel", "given": "Ed" } } ] }, "doi": "10.48550/arXiv.0005364", "primary_object": { "basename": "0005364.pdf", "url": "https://authors.library.caltech.edu/records/1gpae-90w41/files/0005364.pdf" }, "pub_year": "2000", "author_list": "Bildsten, Lars and Rutledge, Robert E." }, { "id": "https://authors.library.caltech.edu/records/va20h-w6p19", "eprint_id": 28168, "eprint_status": "archive", "datestamp": "2023-08-19 03:55:12", "lastmod": "2025-01-29 23:35:50", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blackburn-K", "name": { "family": "Blackburn", "given": "Kent" } }, { "id": "Lazzarini-A", "name": { "family": "Lazzarini", "given": "Albert" } }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627" }, { "id": "Williams-R-D", "name": { "family": "Williams", "given": "Roy" }, "orcid": "0000-0002-9145-8580" } ] }, "title": "XSIL: Extensible Scientific Interchange Language", "ispublished": "unpub", "full_text_status": "public", "abstract": "We motivate and define the XSIL language as a flexible, hierarchical, extensible transport language for scientific data objects. The entire object may be represented in the file, or there may be metadata in the XSIL file, with a powerful, fault-tolerant linking mechanism to external data. The language is based on XML, and is designed not only for parsing and processing by machines, but also for presentation to humans through web browsers and web-database technology. There is a natural mapping between the elements of the XSIL language and the object model into which they are translated by the parser. As well as common objects (Parameter, Array, Time, Table), we have extended XSIL to include the IGWDFrame, used by gravitational-wave observatories.", "date": "1999-01-01", "date_type": "published", "publisher": "California Institute of Technology", "id_number": "CaltechCACR:CACR-1999-171", "official_url": "https://resolver.caltech.edu/CaltechCACR:CACR-1999-171", "rights": "You are granted permission for individual, educational, research and non-commercial reproduction, distribution, display and performance of this work in any format.", "local_group": { "items": [ { "id": "Center-for-Advanced-Computing-Research" }, { "id": "Space-Radiation-Laboratory" } ] }, "primary_object": { "basename": "cacr171.pdf", "url": "https://authors.library.caltech.edu/records/va20h-w6p19/files/cacr171.pdf" }, "pub_year": "1999", "author_list": "Blackburn, Kent; Lazzarini, Albert; et al." }, { "id": "https://authors.library.caltech.edu/records/d1z4v-72j38", "eprint_id": 45089, "eprint_status": "archive", "datestamp": "2023-08-19 16:35:00", "lastmod": "2024-01-13 15:26:40", "type": "monograph", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "E. C." }, "orcid": "0000-0002-2010-5462" } ] }, "title": "The Voyager Encounters with Saturn", "ispublished": "unpub", "full_text_status": "public", "note": "\u00a9 American Institute of Aeronautics and Astronautics, Inc., 1983.\n\nPublished - 1983-01.pdf
", "abstract": "Two Voyager spacecraft were launched in 1977 on a mission of exploration and scientific investigation of the outer solar system. The autonomous spacecraft carried out complex observational sequences of Jupiter and Saturn and their rings, satellites, and magnetospheres. A brief overview of some of the discoveries about the Saturnian system is presented.", "date": "1984-01", "date_type": "published", "publisher": "American Institute of Aeronautics and Astronautics", "id_number": "CaltechAUTHORS:20140421-152926477", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140421-152926477", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "other_numbering_system": { "items": [ { "id": "1983-01", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ { "id": "Space-Radiation-Laboratory" } ] }, "primary_object": { "basename": "1983-01.pdf", "url": "https://authors.library.caltech.edu/records/d1z4v-72j38/files/1983-01.pdf" }, "pub_year": "1984", "author_list": "Stone, E. C." } ]