1,298 results on '"Moseley, S."'
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2. Optimization of an Optical Testbed for Characterization of EXCLAIM u-Spec Integrated Spectrometers
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Rahmani, Maryam, Barrentine, Emily M., Switzer, Eric R., Barlis, Alyssa, Brown, Ari D., Cataldo, Giuseppe, Connors, Jake A., Ehsan, Negar, Essinger-Hileman, Thomas M., Grant, Henry, Hays-Wehle, James, Hsieh, Wen-Ting, Mikula, Vilem, Moseley, S. Harvey, Noroozian, Omid, Quijada, Manuel A., Patel, Jessica, Stevenson, Thomas R., Tucker, Carole, U-Yen, Kongpop, Volpert, Carolyn G., and Wollack, Edward J.
- Subjects
Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We describe a testbed to characterize the optical response of compact superconducting on-chip spectrometers in development for the Experiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) mission. EXCLAIM is a balloonborne far-infrared experiment to probe the CO and CII emission lines in galaxies from redshift 3.5 to the present. The spectrometer, called u-Spec, comprises a diffraction grating on a silicon chip coupled to kinetic inductance detectors (KIDs) read out via a single microwave feedline. We use a prototype spectrometer for EXCLAIM to demonstrate our ability to characterize the spectrometers spectral response using a photomixer source. We utilize an on-chip reference detector to normalize relative to spectral structure from the off-chip optics and a silicon etalon to calibrate the absolute frequency.
- Published
- 2023
3. The James Webb Space Telescope Mission
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Gardner, Jonathan P., Mather, John C., Abbott, Randy, Abell, James S., Abernathy, Mark, Abney, Faith E., Abraham, John G., Abraham, Roberto, Abul-Huda, Yasin M., Acton, Scott, Adams, Cynthia K., Adams, Evan, Adler, David S., Adriaensen, Maarten, Aguilar, Jonathan Albert, Ahmed, Mansoor, Ahmed, Nasif S., Ahmed, Tanjira, Albat, Rüdeger, Albert, Loïc, Alberts, Stacey, Aldridge, David, Allen, Mary Marsha, Allen, Shaune S., Altenburg, Martin, Altunc, Serhat, Alvarez, Jose Lorenzo, Álvarez-Márquez, Javier, de Oliveira, Catarina Alves, Ambrose, Leslie L., Anandakrishnan, Satya M., Andersen, Gregory C., Anderson, Harry James, Anderson, Jay, Anderson, Kristen, Anderson, Sara M., Aprea, Julio, Archer, Benita J., Arenberg, Jonathan W., Argyriou, Ioannis, Arribas, Santiago, Artigau, Étienne, Arvai, Amanda Rose, Atcheson, Paul, Atkinson, Charles B., Averbukh, Jesse, Aymergen, Cagatay, Bacinski, John J., Baggett, Wayne E., Bagnasco, Giorgio, Baker, Lynn L., Balzano, Vicki Ann, Banks, Kimberly A., Baran, David A., Barker, Elizabeth A., Barrett, Larry K., Barringer, Bruce O., Barto, Allison, Bast, William, Baudoz, Pierre, Baum, Stefi, Beatty, Thomas G., Beaulieu, Mathilde, Bechtold, Kathryn, Beck, Tracy, Beddard, Megan M., Beichman, Charles, Bellagama, Larry, Bely, Pierre, Berger, Timothy W., Bergeron, Louis E., Darveau-Bernier, Antoine, Bertch, Maria D., Beskow, Charlotte, Betz, Laura E., Biagetti, Carl P., Birkmann, Stephan, Bjorklund, Kurt F., Blackwood, James D., Blazek, Ronald Paul, Blossfeld, Stephen, Bluth, Marcel, Boccaletti, Anthony, Boegner Jr., Martin E., Bohlin, Ralph C., Boia, John Joseph, Böker, Torsten, Bonaventura, N., Bond, Nicholas A., Bosley, Kari Ann, Boucarut, Rene A., Bouchet, Patrice, Bouwman, Jeroen, Bower, Gary, Bowers, Ariel S., Bowers, Charles W., Boyce, Leslye A., Boyer, Christine T., Boyer, Martha L., Boyer, Michael, Boyer, Robert, Bradley, Larry D., Brady, Gregory R., Brandl, Bernhard R., Brannen, Judith L., Breda, David, Bremmer, Harold G., Brennan, David, Bresnahan, Pamela A., Bright, Stacey N., Broiles, Brian J., Bromenschenkel, Asa, Brooks, Brian H., Brooks, Keira J., Brown, Bob, Brown, Bruce, Brown, Thomas M., Bruce, Barry W., Bryson, Jonathan G., Bujanda, Edwin D., Bullock, Blake M., Bunker, A. J., Bureo, Rafael, Burt, Irving J., Bush, James Aaron, Bushouse, Howard A., Bussman, Marie C., Cabaud, Olivier, Cale, Steven, Calhoon, Charles D., Calvani, Humberto, Canipe, Alicia M., Caputo, Francis M., Cara, Mihai, Carey, Larkin, Case, Michael Eli, Cesari, Thaddeus, Cetorelli, Lee D., Chance, Don R., Chandler, Lynn, Chaney, Dave, Chapman, George N., Charlot, S., Chayer, Pierre, Cheezum, Jeffrey I., Chen, Bin, Chen, Christine H., Cherinka, Brian, Chichester, Sarah C., Chilton, Zachary S., Chittiraibalan, Dharini, Clampin, Mark, Clark, Charles R., Clark, Kerry W., Clark, Stephanie M., Claybrooks, Edward E., Cleveland, Keith A., Cohen, Andrew L., Cohen, Lester M., Colón, Knicole D., Coleman, Benee L., Colina, Luis, Comber, Brian J., Comeau, Thomas M., Comer, Thomas, Reis, Alain Conde, Connolly, Dennis C., Conroy, Kyle E., Contos, Adam R., Contreras, James, Cook, Neil J., Cooper, James L., Cooper, Rachel Aviva, Correia, Michael F., Correnti, Matteo, Cossou, Christophe, Costanza, Brian 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Kimberly C., Dupuis, Jean, Durning, John, Dutta, Sanghamitra B., Earl, Nicholas M., Eccleston, Paul, Ecobichon, Pascal, Egami, Eiichi, Ehrenwinkler, Ralf, Eisenhamer, Jonathan D., Eisenhower, Michael, Eisenstein, Daniel J., Hamel, Zaky El, Elie, Michelle L., Elliott, James, Elliott, Kyle Wesley, Engesser, Michael, Espinoza, Néstor, Etienne, Odessa, Etxaluze, Mireya, Evans, Leah, Fabreguettes, Luce, Falcolini, Massimo, Falini, Patrick R., Fatig, Curtis, Feeney, Matthew, Feinberg, Lee D., Fels, Raymond, Ferdous, Nazma, Ferguson, Henry C., Ferrarese, Laura, Ferreira, Marie-Héléne, Ferruit, Pierre, Ferry, Malcolm, Filippazzo, Joseph Charles, Firre, Daniel, Fix, Mees, Flagey, Nicolas, Flanagan, Kathryn A., Fleming, Scott W., Florian, Michael, Flynn, James R., Foiadelli, Luca, Fontaine, Mark R., Fontanella, Erin Marie, Forshay, Peter Randolph, Fortner, Elizabeth A., Fox, Ori D., Framarini, Alexandro P., Francisco, John I., Franck, Randy, Franx, Marijn, Franz, David E., Friedman, Scott D., Friend, Katheryn E., Frost, James R., Fu, Henry, Fullerton, Alexander W., Gaillard, Lionel, Galkin, Sergey, Gallagher, Ben, Galyer, Anthony D., Marín, Macarena García, Gardner, Lisa E., Garland, Dennis, Garrett, Bruce Albert, Gasman, Danny, Gáspár, András, Gastaud, René, Gaudreau, Daniel, Gauthier, Peter Timothy, Geers, Vincent, Geithner, Paul H., Gennaro, Mario, Gerber, John, Gereau, John C., Giampaoli, Robert, Giardino, Giovanna, Gibbons, Paul C., Gilbert, Karolina, Gilman, Larry, Girard, Julien H., Giuliano, Mark E., Gkountis, Konstantinos, Glasse, Alistair, Glassmire, Kirk Zachary, Glauser, Adrian Michael, Glazer, Stuart D., Goldberg, Joshua, Golimowski, David A., Gonzaga, Shireen P., Gordon, Karl D., Gordon, Shawn J., Goudfrooij, Paul, Gough, Michael J., Graham, Adrian J., Grau, Christopher M., Green, Joel David, Greene, Gretchen R., Greene, Thomas P., Greenfield, Perry E., Greenhouse, Matthew A., Greve, Thomas R., Greville, Edgar M., Grimaldi, Stefano, Groe, Frank E., Groebner, 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Jurkowski, Mark H., Justis, Grant, Justtanont, Kay, Kaleida, Catherine C., Kalirai, Jason S., Kalmanson, Phillip Cabrales, Kaltenegger, Lisa, Kammerer, Jens, Kan, Samuel K., Kanarek, Graham Childs, Kao, Shaw-Hong, Karakla, Diane M., Karl, Hermann, Kassin, Susan A., Kauffman, David D., Kavanagh, Patrick, Kelley, Leigh L., Kelly, Douglas M., Kendrew, Sarah, Kennedy, Herbert V., Kenny, Deborah A., Keski-Kuha, Ritva A., Keyes, Charles D., Khan, Ali, Kidwell, Richard C., Kimble, Randy A., King, James S., King, Richard C., Kinzel, Wayne M., Kirk, Jeffrey R., Kirkpatrick, Marc E., Klaassen, Pamela, Klingemann, Lana, Klintworth, Paul U., Knapp, Bryan Adam, Knight, Scott, Knollenberg, Perry J., Knutsen, Daniel Mark, Koehler, Robert, Koekemoer, Anton M., Kofler, Earl T., Kontson, Vicki L., Kovacs, Aiden Rose, Kozhurina-Platais, Vera, Krause, Oliver, Kriss, Gerard A., Krist, John, Kristoffersen, Monica R., Krogel, Claudia, Krueger, Anthony P., Kulp, Bernard A., Kumari, Nimisha, Kwan, Sandy W., 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A., Willott, Chris J., Willoughby, Scott P., Wilson, Andrew, Wilson, Debra, Wilson, Donna V., Windhorst, Rogier, Wislowski, Emily Christine, Wolfe, David J., Wolfe, Michael A., Wolff, Schuyler, Wondel, Amancio, Woo, Cindy, Woods, Robert T., Worden, Elaine, Workman, William, Wright, Gillian S., Wu, Carl, Wu, Chi-Rai, Wun, Dakin D., Wymer, Kristen B., Yadetie, Thomas, Yan, Isabelle C., Yang, Keith C., Yates, Kayla L., Yeager, Christopher R., Yerger, Ethan John, Young, Erick T., Young, Gary, Yu, Gene, Yu, Susan, Zak, Dean S., Zeidler, Peter, Zepp, Robert, Zhou, Julia, Zincke, Christian A., Zonak, Stephanie, and Zondag, Elisabeth
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 years, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit., Comment: Accepted by PASP for the special issue on The James Webb Space Telescope Overview, 29 pages, 4 figures
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- 2023
- Full Text
- View/download PDF
4. In-orbit Performance of the Near-Infrared Spectrograph NIRSpec on the James Webb Space Telescope
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Böker, T., Beck, T. L., Birkmann, S. M., Giardino, G., Keyes, C., Kumari, N., Muzerolle, J., Rawle, T., Zeidler, P., Abul-Huda, Y., de Oliveira, C. Alves, Arribas, S., Bechtold, K., Bhatawdekar, R., Bonaventura, N., Bunker, A. J., Cameron, A. J., Carniani, S., Charlot, S., Curti, M., Espinoza, N., Ferruit, P., Franx, M., Jakobsen, P., Karakla, D., López-Caniego, M., Lützgendorf, N., Maiolino, R., Manjavacas, E., Marston, A. P., Moseley, S. H., Ogle, P., Perna, M., Peña-Guerrero, M., Pirzkal, N., Plesha, R., Proffitt, C. R., Rauscher, B. J., Rix, H. -W., del Pino, B. Rodríguez, Rustamkulov, Z., Sabbi, E., Sing, D. K., Sirianni, M., Plate, M. te, Úbeda, L., Wahlgren, G. M., Wislowski, E., Wu, R., and Willott, C. J.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Near-Infrared Spectrograph (NIRSpec) is one of the four focal plane instruments on the James Webb Space Telescope. In this paper, we summarize the in-orbit performance of NIRSpec, as derived from data collected during its commissioning campaign and the first few months of nominal science operations. More specifically, we discuss the performance of some critical hardware components such as the two NIRSpec Hawaii-2RG (H2RG) detectors, wheel mechanisms, and the micro-shutter array. We also summarize the accuracy of the two target acquisition procedures used to accurately place science targets into the slit apertures, discuss the current status of the spectro-photometric and wavelength calibration of NIRSpec spectra, and provide the as measured sensitivity in all NIRSpec science modes. Finally, we point out a few important considerations for the preparation of NIRSpec science programs., Comment: accepted by PASP for special issue on JWST in-orbit performance
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- 2023
- Full Text
- View/download PDF
5. Optical Characterization & Testbed Development for {\mu}-Spec Integrated Spectrometers
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Rahmani, Maryam, Barlis, Alyssa, Barrentine, Emily M., Brown, Ari D., Bulcha, Berhanu T., Cataldo, Giuseppe, Connors, Jake, Ehsan, Negar, Essinger-Hileman, Thomas M., Grant, Henry, Hays-Wehle, James, Hsieh, Wen-Ting, Mikula, Vilem, Moseley, S. Harvey, Noroozian, Omid, Oxholm, Trevor R., Quijada, Manuel A., Patel, Jessica, Stevenson, Thomas R., Switzer, Eric R., Tucker, Carole, U-Yen, Kongpop, Volpert, Carolyn, and Wollack, Edward J.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
This paper describes a cryogenic optical testbed developed to characterize u-Spec spectrometers in a dedicated dilution refrigerator (DR) system. u-Spec is a far-infrared integrated spectrometer that is an analog to a Rowland-type grating spectrometer. It employs a single-crystal silicon substrate with niobium microstrip lines and aluminum kinetic inductance detectors (KIDs). Current designs with a resolution of 512 are in fabrication for the EXCLAIM (Experiment for Cryogenic Large Aperture Intensity Mapping) balloon mission. The primary spectrometer performance and design parameters are efficiency, NEP, inter-channel isolation, spectral resolution, and frequency response for each channel. Here we present the development and design of an optical characterization facility and preliminary validation of that facility with earlier prototype R=64 devices. We have conducted and describe initial optical measurements of R = 64 devices using a swept photomixer line source. We also discuss the test plan for optical characterization of the EXCLAIM R = 512 u-Spec devices in this new testbed., Comment: SPIE conference, Montreal, Ca. July 17-22, 2022
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- 2022
6. In-flight performance of the NIRSpec Micro Shutter Array
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Rawle, Timothy D., Giardino, Giovanna, Franz, David E., Rapp, Robert, Plate, Maurice te, Zincke, Christian A., Abul-Huda, Yasin M., de Oliveira, Catarina Alves, Bechtold, Katie, Beck, Tracy, Birkmann, Stephan M., Böker, Torsten, Ehrenwinkler, Ralf, Ferruit, Pierre, Garland, Dennis, Jakobsen, Peter, Karakla, Diane, Karl, Hermann, Keyes, Charles D., Koehler, Robert, Kumari, Nimisha, Lützgendorf, Nora, Manjavacas, Elena, Marston, Anthony, Moseley, S. Harvey, Mosner, Peter, Muzerolle, James, Ogle, Patrick, Proffitt, Charles, Sabbi, Elena, Sirianni, Marco, Wahlgren, Glenn, Wislowski, Emily, Wright, Raymond H., Wu, Chi Rai, and Zeidler, Peter
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The NIRSpec instrument on the James Webb Space Telescope (JWST) brings the first multi-object spectrograph (MOS) into space, enabled by a programmable Micro Shutter Array (MSA) of ~250,000 individual apertures. During the 6-month Commissioning period, the MSA performed admirably, completing ~800 reconfigurations with an average success rate of ~96% for commanding shutters open in science-like patterns. We show that 82.5% of the unvignetted shutter population is usable for science, with electrical short masking now the primary cause of inoperable apertures. In response, we propose a plan to recheck existing shorts during nominal operations, which is expected to reduce the number of affected shutters. We also present a full assessment of the Failed Open and Failed Closed shutter populations, which both show a marginal increase in line with predictions from ground testing. We suggest an amendment to the Failed Closed shutter flagging scheme to improve flexibility for MSA configuration planning. Overall, the NIRSpec MSA performed very well during Commissioning, and the MOS mode was declared ready for science operations on schedule., Comment: 15 pages, 6 figures, to appear in Proceedings of SPIE conference "Space Telescopes and Instrumentation 2022: Optical, Infrared, and Millimeter Wave"
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- 2022
7. Dual-Resonator Kinetic-Inductance Detector for Distinction between Signal and 1/f Frequency Noise
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Foroozani, N., Sarabi, B., Moseley, S. H., Stevenson, T., Wollack, E. J., Noroozian, O., and Osborn, K. D.
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Condensed Matter - Superconductivity ,Quantum Physics - Abstract
Astronomical Kinetic Inductance Detectors (KIDs), similar to quantum information devices, experience performance limiting noise from materials. In particular, 1/f (frequency) noise can be a dominant noise mechanism, which arises from Two-Level System defects (TLSs) in the circuit dielectrics and material interfaces. Here we present a Dual-Resonator KID (DuRKID), which is designed for improved signal to noise (or noise equivalent power) relative to 1/f-noise limited KIDs. We first show the DuRKID schematic, fabricated circuit, and we follow with a description of the intended operation, first measurements, theory, and discussion. The circuit consists of two superconducting resonators sharing an electrical capacitance bridge of 4 capacitors, each of which hosts TLSs. The device is intended to operate using hybridization of the modes, which causes TLSs to either couple to one mode or the other, depending upon which capacitor they reside in. In contrast, the intended KID signal is directed to an inductor, and due to hybridization this causes correlated frequency changes in both (hybridized) modes. Therefore, one can distinguish photon signal from TLS frequency noise. To achieve hybridization, a TiN inductor is current biased to allow tuning of one bare resonator mode into degeneracy with the other and measurements show that the intended resonator modes frequency tune and hybridize as expected. The interresonator coupling and unintentional coupling of the 2 resonators to transmission lines are also characterized in measurements. In the theory, based on a quantum-information-science modes, we calculate the 4-port S parameters and simulate the 1/f frequency noise of the device. The study reveals that the DuRKID can exhibit a large and fundamental performance advantage over 1/f-noise-limited KID detectors., Comment: 20 pages, 12 figures
- Published
- 2022
8. The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope IV. Capabilities and predicted performance for exoplanet characterization
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Birkmann, S. M., Ferruit, P., Giardino, G., Nielsen, L. D., Muñoz, A. García, Kendrew, S., Rauscher, B. J., Beck, T. L., Keyes, C., Valenti, J. A., Jakobsen, P., Dorner, B., de Oliveira, C. Alves, Arribas, S., Böker, T., Bunker, A. J., Charlot, S., de Marchi, G., Kumari, N., López-Caniego, M., Lützgendorf, N., Maiolino, R., Manjavacas, E., Marston, A., Moseley, S. H., Prizkal, N., Proffitt, C., Rawle, T., Rix, H. W., Plate, M. te, Sabbi, E., Sirianni, M., Willott, C. J., and Zeidler, P.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The Near-Inrared Spectrograph (NIRSpec) on the James Webb Space Telescope (JWST) is a very versatile instrument, offering multiobject and integral field spectroscopy with varying spectral resolution ($\sim$30 to $\sim$3000) over a wide wavelength range from 0.6 to 5.3 micron, enabling scientists to study many science themes ranging from the first galaxies to bodies in our own Solar System. In addition to its integral field unit and support for multiobject spectroscopy, NIRSpec features several fixed slits and a wide aperture specifically designed to enable high precision time-series and transit as well as eclipse observations of exoplanets. In this paper we present its capabilities regarding time-series observations, in general, and transit and eclipse spectroscopy of exoplanets in particular. Due to JWST's large collecting area and NIRSpec's excellent throughput, spectral coverage, and detector performance, this mode will allow scientists to characterize the atmosphere of exoplanets with unprecedented sensitivity., Comment: Accepted for publication in A&A. 15 pages, 15 figures
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- 2022
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9. The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope III. Integral-field spectroscopy
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Böker, T., Arribas, S., Lützgendorf, N., de Oliveira, C. Alves, Beck, T. L., Birkmann, S., Bunker, A. J., Charlot, S., de Marchi, G., Ferruit, P., Giardino, G., Jakobsen, P., Kumari, N., López-Caniego, M., Maiolino, R., Manjavacas, E., Marston, A., Moseley, S. H., Muzerolle, J., Ogle, P., Pirzkal, N., Rauscher, B., Rawle, T., Rix, H. W., Sabbi, E., Sargent, B., Sirianni, M., Plate, M. te, Valenti, J., Willott, C. J., and Zeidler, P.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope (JWST) offers the first opportunity to use integral-field spectroscopy from space at near-infrared wavelengths. More specifically, NIRSpec's integral-field unit can obtain spectra covering the wavelength range $0.6 - 5.3~\mu$m for a contiguous 3.1 arcsec $\times$ 3.2 arcsec sky area at spectral resolutions of $R \approx 100$, 1000, and 2700. In this paper we describe the optical and mechanical design of the NIRSpec integral-field spectroscopy mode, together with its expected performance. We also discuss a few recommended observing strategies, some of which are driven by the fact that NIRSpec is a multipurpose instrument with a number of different observing modes, which are discussed in companion papers. We briefly discuss the data processing steps required to produce wavelength- and flux-calibrated data cubes that contain the spatial and spectral information. Lastly, we mention a few scientific topics that are bound to benefit from this highly innovative capability offered by JWST/NIRSpec., Comment: Accepted for publication in A&A. 13 pages, 14 figures
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- 2022
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10. The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope II. Multi-object spectroscopy (MOS)
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Ferruit, P., Jakobsen, P., Giardino, G., Rawle, T., de Oliveira, C. Alves, Arribas, S., Beck, T. L., Birkmann, S., Böker, T., Bunker, A. J., Charlot, S., de Marchi, G., Franx, M., Henry, A., Karakla, D., Kassin, S. A., Kumari, N., López-Caniego, M., Lützgendorf, N., Maiolino, R., Manjavacas, E., Marston, A., Moseley, S. H., Muzerolle, J., Pirzkal, N., Rauscher, B., Rix, H. W., Sabbi, E., Sirianni, M., Plate, M. te, Valenti, J., Willott, C. J., and Zeidler, P.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We provide an overview of the capabilities and performance of the Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope (JWST) when used in its multi-object spectroscopy (MOS) mode employing a novel Micro Shutter Array (MSA) slit device. The MSA consists of four separate 98 arcsec $\times$ 91 arcsec quadrants each containing $365\times171$ individually addressable shutters whose open areas on the sky measure 0.20 arcsec $\times$ 0.46 arcsec on a 0.27 arcsec $\times$ 0.53 arcsec pitch. This is the first time that a configurable multi-object spectrograph has been available on a space mission. The levels of multiplexing achievable with NIRSpec MOS mode are quantified and we show that NIRSpec will be able to observe typically fifty to two hundred objects simultaneously with the pattern of close to a quarter of a million shutters provided by the MSA. This pattern is fixed and regular, and we identify the specific constraints that it yields for NIRSpec observation planning. We also present the data processing and calibration steps planned for the NIRSpec MOS data. The significant variation in size of the mostly diffraction-limited instrument point spread function over the large wavelength range of 0.6-5.3 $\mu$m covered by the instrument, combined with the fact that most targets observed with the MSA cannot be expected to be perfectly centred within their respective slits, makes the spectrophotometric and wavelength calibration of the obtained spectra particularly complex. These challenges notwithstanding, the sensitivity and multiplexing capabilities anticipated of NIRSpec in MOS mode are unprecedented, and should enable significant progress to be made in addressing a wide range of outstanding astrophysical problems., Comment: Accepted for publication in A&A. 16 pages, 14 figure
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- 2022
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11. The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope I. Overview of the instrument and its capabilities
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Jakobsen, P., Ferruit, P., de Oliveira, C. Alves, Arribas, S., Bagnasco, G., Barho, R., Beck, T. L., Birkmann, S., Böker, T., Bunker, A. J., Charlot, S., de Jong, P., de Marchi, G., Ehrenwinkler, R., Falcolini, M., Fels, R., Franx, M., Franz, D., Funke, M., Giardino, G., Gnata, X., Holota, W., Honnen, K., Jensen, P. L., Jentsch, M., Johnson, T., Jollet, D., Karl, H., Kling, G., Köhler, J., Kolm, M. G., Kumari, N., Lander, M. E., Lemke, R., López-Caniego, M., Lützgendorf, N., Maiolino, R., Manjavacas, E., Marston, A., Maschmann, M., Maurer, R., Messerschmidt, B., Moseley, S. H., Mosner, P., Mott, D. B., Muzerolle, J., Pirzkal, N., Pittet, J. F., Plitzke, A., Posselt, W., Rapp, B., Rauscher, B. J., Rawle, T., Rix, H. W., Rödel, A., Rumler, P., Sabbi, E., Salvignol, J. C., Schmid, T., Sirianni, M., Smith, C., Strada, P., Plate, M. te, Valenti, J., Wettemann, T., Wiehe, T., Wiesmayer, M., Willott, C. J., Wright, R., Zeidler, P., and Zincke, C.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We provide an overview of the design and capabilities of the near-infrared spectrograph (NIRSpec) onboard the James Webb Space Telescope. NIRSpec is designed to be capable of carrying out low-resolution ($R\!=30\!-330$) prism spectroscopy over the wavelength range $0.6-5.3\!~\mu$m and higher resolution ($R\!=500\!-1340$ or $R\!=1320\!-3600$) grating spectroscopy over $0.7-5.2\!~\mu$m, both in single-object mode employing any one of five fixed slits, or a 3.1$\times$3.2 arcsec$^2$ integral field unit, or in multiobject mode employing a novel programmable micro-shutter device covering a 3.6$\times$3.4~arcmin$^2$ field of view. The all-reflective optical chain of NIRSpec and the performance of its different components are described, and some of the trade-offs made in designing the instrument are touched upon. The faint-end spectrophotometric sensitivity expected of NIRSpec, as well as its dependency on the energetic particle environment that its two detector arrays are likely to be subjected to in orbit are also discussed., Comment: Accepted for publication in A&A. 22 pages, 19 figures
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- 2022
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12. Simple, compact, high-resolution monochromatic x-ray source for characterization of x-ray calorimeter arrays
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Leutenegger, M. A., Eckart, M. E., Moseley, S. J., Rohrbach, S. O., Black, J. K., Chiao, M. P., Kelley, R. L., Kilbourne, C. A., and Porter, F. S.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Physics - Instrumentation and Detectors - Abstract
X-ray calorimeters routinely achieve very high spectral resolution, typically a few eV full width at half maximum (FWHM). Measurements of calorimeter line shapes are usually dominated by the natural linewidth of most laboratory calibration sources. This compounds the data acquisition time necessary to statistically sample the instrumental line broadening, and can add systematic uncertainty if the intrinsic line shape of the source is not well known. To address these issues, we have built a simple, compact monochromatic x-ray source using channel cut crystals. A commercial x-ray tube illuminates a pair of channel cut crystals which are aligned in a dispersive configuration to select the \kaone line of the x-ray tube anode material. The entire device, including x-ray tube, can be easily hand carried by one person and may be positioned manually or using a mechanical translation stage. The output monochromatic beam provides a collimated image of the anode spot with magnification of unity in the dispersion direction (typically 100-200 $\mu$m for the x-ray tubes used here), and is unfocused in the cross-dispersion direction, so that the source image in the detector plane appears as a line. We measured output count rates as high as 10 count/s/pixel for the Hitomi Soft X-ray Spectrometer, which had 819 $\mu$m square pixels. We implemented different monochromator designs for energies of 5.4 keV (one design) and 8.0 keV (two designs) which have effective theoretical FWHM energy resolution of 0.125, 0.197, and 0.086 eV, respectively; these are well-suited for optimal calibration measurements of state-of-the art x-ray calorimeters. We measured an upper limit for the energy resolution of our \crkaone monochromator of 0.7 eV FWHM at 5.4 keV, consistent with the theoretical prediction of 0.125 eV., Comment: 14 pages, 15 figures, accepted for publication in RSI
- Published
- 2020
13. The Experiment for Cryogenic Large-aperture Intensity Mapping (EXCLAIM)
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Ade, P. A. R., Anderson, C. J., Barrentine, E. M., Bellis, N. G., Bolatto, A. D., Breysse, P. C., Bulcha, B. T., Cataldo, G., Connors, J. A., Cursey, P. W., Ehsan, N., Grant, H. C., Essinger-Hileman, T. M., Hess, L. A., Kimball, M. O., Kogut, A. J., Lamb, A. D., Lowe, L. N., Mauskopf, P. D., McMahon, J., Mirzaei, M., Moseley, S. H., Mugge-Durum, J. W., Noroozian, O., Pen, U., Pullen, A. R., Rodriguez, S., Shirron, P. J., Somerville, R. S., Stevenson, T. R., Switzer, E. R., Tucker, C., Visbal, E., Volpert, C. G., Wollack, E. J., and Yang, S.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) is a cryogenic balloon-borne instrument that will survey galaxy and star formation history over cosmological time scales. Rather than identifying individual objects, EXCLAIM will be a pathfinder to demonstrate an intensity mapping approach, which measures the cumulative redshifted line emission. EXCLAIM will operate at 420-540 GHz with a spectral resolution R=512 to measure the integrated CO and [CII] in redshift windows spanning 0 < z < 3.5. CO and [CII] line emissions are key tracers of the gas phases in the interstellar medium involved in star-formation processes. EXCLAIM will shed light on questions such as why the star formation rate declines at z < 2, despite continued clustering of the dark matter. The instrument will employ an array of six superconducting integrated grating-analog spectrometers (micro-spec) coupled to microwave kinetic inductance detectors (MKIDs). Here we present an overview of the EXCLAIM instrument design and status., Comment: 10 pages, 4 figures
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- 2019
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14. Origins Space Telescope Mission Concept Study Report
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Meixner, M., Cooray, A., Leisawitz, D., Staguhn, J., Armus, L., Battersby, C., Bauer, J., Bergin, E., Bradford, C. M., Ennico-Smith, K., Fortney, J., Kataria, T., Melnick, G., Milam, S., Narayanan, D., Padgett, D., Pontoppidan, K., Pope, A., Roellig, T., Sandstrom, K., Stevenson, K., Su, K., Vieira, J., Wright, E., Zmuidzinas, J., Sheth, K., Benford, D., Mamajek, E. E., Neff, S., De Beck, E., Gerin, M., Helmich, F., Sakon, I., Scott, D., Vavrek, R., Wiedner, M., Carey, S., Burgarella, D., Moseley, S. H., Amatucci, E., Carter, R. C., DiPirro, M., Wu, C., Beaman, B., Beltran, P., Bolognese, J., Bradley, D., Corsetti, J., D'Asto, T., Denis, K., Derkacz, C., Earle, C. P., Fantano, L. G., Folta, D., Gavares, B., Generie, J., Hilliard, L., Howard, J. M., Jamil, A., Jamison, T., Lynch, C., Martins, G., Petro, S., Ramspacher, D., Rao, A., Sandin, C., Stoneking, E., Tompkins, S., and Webster, C.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
The Origins Space Telescope (Origins) traces our cosmic history, from the formation of the first galaxies and the rise of metals to the development of habitable worlds and present-day life. Origins does this through exquisite sensitivity to infrared radiation from ions, atoms, molecules, dust, water vapor and ice, and observations of extra-solar planetary atmospheres, protoplanetary disks, and large-area extragalactic fields. Origins operates in the wavelength range 2.8 to 588 microns and is 1000 times more sensitive than its predecessors due to its large, cold (4.5 K) telescope and advanced instruments. Origins was one of four large missions studied by the community with support from NASA and industry in preparation for the 2020 Decadal Survey in Astrophysics. This is the final study report., Comment: 376 pages
- Published
- 2019
15. Sub-Kelvin cooling for two kilopixel bolometer arrays in the PIPER receiver
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Switzer, E. R., Ade, P. A. R., Baildon, T., Benford, D., Bennett, C. L., Chuss, D. T., Datta, R., Eimer, J. R., Fixsen, D. J., Gandilo, N. N., Essinger-Hileman, T. M., Halpern, M., Hilton, G., Irwin, K., Jhabvala, C., Kimball, M., Kogut, A., Lazear, J., Lowe, L. N., McMahon, J. J., Miller, T. M., Mirel, P., Moseley, S. H., Pawlyk, S., Rodriguez, S., Sharp, E., Shirron, P., Staguhn, J. G., Sullivan, D. F., Taraschi, P., Tucker, C. E., Walts, A., and Wollack, E. J.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Primordial Inflation Polarization Explorer (PIPER) is a balloon-borne telescope mission to search for inflationary gravitational waves from the early universe. PIPER employs two 32x40 arrays of superconducting transition-edge sensors, which operate at 100 mK. An open bucket dewar of liquid helium maintains the receiver and telescope optics at 1.7 K. We describe the thermal design of the receiver and sub-kelvin cooling with a continuous adiabatic demagnetization refrigerator (CADR). The CADR operates between 70-130 mK and provides ~10 uW cooling power at 100 mK, nearly five times the loading of the two detector assemblies. We describe electronics and software to robustly control the CADR, overall CADR performance in flight-like integrated receiver testing, and practical considerations for implementation in the balloon float environment., Comment: 14 pages, 12 figures
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- 2019
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16. Principal Component Analysis of Up-the-ramp Sampled IR Array Data
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Rauscher, Bernard J., Arendt, Richard G., Fixsen, D. J., Kutyrev, Alexander, Mosby, Gregory, and Moseley, S. H.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We describe the results of principal component analysis (PCA) of up-the-ramp sampled IR array data from the HST WFC3 IR, JWST NIRSpec, and prototype WFIRST WFI detectors. These systems use respectively Teledyne H1R, H2RG, and H4RG-10 near-IR detector arrays with a variety of IR array controllers. The PCA shows that the Legendre polynomials approximate the principal components of these systems (i.e. they roughly diagonalize the covariance matrix). In contrast to the monomial basis that is widely used for polynomial fitting and linearization today, the Legendre polynomials are an orthonormal basis. They provide a quantifiable, compact, and (nearly) linearly uncorrelated representation of the information content of the data. By fitting a few Legendre polynomials, nearly all of the meaningful information in representative WFC3 astronomical datacubes can be condensed from 15 up-the-ramp samples down to 6 compressible Legendre coefficients per pixel. The higher order coefficients contain time domain information that is lost when one projects up-the-ramp sampled datacubes onto 2-dimensional images by fitting a straight line, even if the data are linearized before fitting the line. Going forward, we believe that this time domain information is potentially important for disentangling the various non-linearities that can affect IR array observations, i.e. inherent pixel non-linearity, persistence, burn in, brighter-fatter effect, (potentially) non-linear inter-pixel capacitance (IPC), and perhaps others., Comment: 26 pages, 10 figures, accepted by Journal of Astronomical Telescopes, Instruments, and Systems (JATIS)
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- 2019
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17. HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1
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Chuss, David T., Andersson, B-G, Bally, John, Dotson, Jessie L., Dowell, C. Darren, Guerra, Jordan A., Harper, Doyal A., Houde, Martin, Jones, Terry Jay, Lazarian, A., Rodriguez, Enrique Lopez, Michail, Joseph M., Morris, Mark R., Novak, Giles, Siah, Javad, Staguhn, Johannes, Vaillancourt, John E., Volpert, C. G., Werner, Michael, Wollack, Edward J., Benford, Dominic J., Berthoud, Marc, Cox, Erin G., Crutcher, Richard, Dale, Daniel A., Fissel, L. M., Goldsmith, Paul F., Hamilton, Ryan T., Hanany, Shaul, Henning, Thomas K., Looney, Leslie W., Moseley, S. Harvey, Santos, Fabio P., Stephens, Ian, Tassis, Konstantinos, Trinh, Christopher Q., Van Camp, Eric, and Ward-Thompson, Derek
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Astrophysics - Astrophysics of Galaxies - Abstract
We report new polarimetric and photometric maps of the massive star-forming region OMC-1 using the HAWC+ instrument on the Stratospheric Observatory for Infrared Astronomy (SOFIA). We present continuum polarimetric and photometric measurements of this region at 53, 89, 154, and 214 microns at angular resolutions of 5.1, 7.9, 14.0, and 18.7 arcseconds for the four bands, respectively. The photometric maps enable the computation of improved SEDs for the region. We find that at the longer wavelengths, the inferred magnetic field configuration matches the `hourglass' configuration seen in previous studies, indicating magnetically-regulated star formation. The field morphology differs at the shorter wavelengths. The magnetic field inferred at these wavelengths traces the bipolar structure of the explosive Becklin-Neugebauer (BN)/Kleinman-Low (KL) outflow emerging from OMC-1 behind the Orion Nebula. Using statistical methods to estimate the field strength in the region, we find that the explosion dominates the magnetic field near the center of the feature. Farther out, the magnetic field is close to energetic equilibrium with the ejecta and may be providing confinement to the explosion. The correlation between polarization fraction and the local polarization angle dispersion indicates that the depolarization as a function of unpolarized intensity is a result of intrinsic field geometry as opposed to decreases in grain alignment efficiency in denser regions., Comment: 28 pages, 14 figures, ApJ, accepted
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- 2018
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18. The Origins Space Telescope
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Battersby, Cara, Armus, Lee, Bergin, Edwin, Kataria, Tiffany, Meixner, Margaret, Pope, Alexandra, Stevenson, Kevin B., Cooray, Asantha, Leisawitz, David, Scott, Douglas, Bauer, James, Bradford, C. Matt, Ennico, Kimberly, Fortney, Jonathan J., Kaltenegger, Lisa, Melnick, Gary J., Milam, Stefanie N., Narayanan, Desika, Padgett, Deborah, Pontoppidan, Klaus, Roellig, Thomas, Sandstrom, Karin, Su, Kate Y. L., Vieira, Joaquin, Wright, Edward, Zmuidzinas, Jonas, Staguhn, Johannes, Sheth, Kartik, Benford, Dominic, Mamajek, Eric E., Neff, Susan G., Carey, Sean, Burgarella, Denis, De Beck, Elvire, Gerin, Maryvonne, Helmich, Frank P., Moseley, S. Harvey, Sakon, Itsuki, and Wiedner, Martina C.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The Origins Space Telescope, one of four large Mission Concept studies sponsored by NASA for review in the 2020 US Astrophysics Decadal Survey, will open unprecedented discovery space in the infrared, unveiling our cosmic origins. We briefly describe in this article the key science themes and architecture for OST. With a sensitivity gain of up to a factor of 1,000 over any previous or planned mission, OST will open unprecedented discovery space, allow us to peer through an infrared window teeming with possibility. OST will fundamentally change our understanding of our cosmic origins - from the growth of galaxies and black holes, to uncovering the trail of water, to life signs in nearby Earth-size planets, and discoveries never imagined. Built to be highly adaptable, while addressing key science across many areas of astrophysics, OST will usher in a new era of infrared astronomy., Comment: Published in Nature Astronomy. This 7-page PDF is the submitted version - here is a free link to the published article: https://rdcu.be/3Rtt
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- 2018
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19. Review: Far-Infrared Instrumentation and Technology Development for the Next Decade
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Farrah, Duncan, Smith, Kimberly Ennico, Ardila, David, Bradford, Charles M., Dipirro, Michael, Ferkinhoff, Carl, Glenn, Jason, Goldsmith, Paul, Leisawitz, David, Nikola, Thomas, Rangwala, Naseem, Rinehart, Stephen A., Staguhn, Johannes, Zemcov, Michael, Zmuidzinas, Jonas, Bartlett, James, Carey, Sean, Fischer, William J., Kamenetzky, Julia, Kartaltepe, Jeyhan, Lacy, Mark, Lis, Dariusz C., Locke, Lisa, Lopez-Rodriguez, Enrique, MacGregor, Meredith, Mills, Elisabeth, Moseley, S. Harvey, Murphy, Eric J., Rhodes, Alan, Richter, Matt, Rigopoulou, Dimitra, Sanders, David, Sankrit, Ravi, Savini, Giorgio, Smith, John-David, and Stierwalt, Sabrina
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Astrophysics - Instrumentation and Methods for Astrophysics ,Physics - Instrumentation and Detectors - Abstract
Far-infrared astronomy has advanced rapidly since its inception in the late 1950's, driven by a maturing technology base and an expanding community of researchers. This advancement has shown that observations at far-infrared wavelengths are important in nearly all areas of astrophysics, from the search for habitable planets and the origin of life, to the earliest stages of galaxy assembly in the first few hundred million years of cosmic history. The combination of a still developing portfolio of technologies, particularly in the field of detectors, and a widening ensemble of platforms within which these technologies can be deployed, means that far-infrared astronomy holds the potential for paradigm-shifting advances over the next decade. In this review, we examine current and future far-infrared observing platforms, including ground-based, sub-orbital, and space-based facilities, and discuss the technology development pathways that will enable and enhance these platforms to best address the challenges facing far-infrared astronomy in the 21st century., Comment: Invited review article, submitted to the Journal of Astronomical Telescopes, Instruments, and Systems. Updated in light of referee reports
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- 2017
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20. Improved Reference Sampling and Subtraction: A Technique for Reducing the Read Noise of Near-infrared Detector Systems
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Rauscher, Bernard J., Arendt, Richard G., Fixsen, D. J., Greenhouse, Matthew A., Lander, Matthew, Lindler, Don, Loose, Markus, Moseley, S. H., Mott, D. Brent, Went, Yiting, Wilson, Donna V., and Xenophontos, Christos
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Near-infrared array detectors, like the \JWST NIRSpec's Teledyne's H2RGs, often provide reference pixels and a reference output. These are used to remove correlated noise. Improved Reference Sampling and Subtraction (\IRSSquare, pronounced "IRS-square") is a statistical technique for using this reference information optimally in a least squares sense. Compared to "traditional" H2RG readout, \IRSSquare uses a different clocking pattern to interleave many more reference pixels into the data than is otherwise possible. Compared to standard reference correction techniques, \IRSSquare subtracts the reference pixels and reference output using a statistically optimized set of frequency dependent weights. The benefits include somewhat lower noise variance and much less obvious correlated noise. NIRSpec's \IRSSquare images are cosmetically clean, with less $1/f$ banding than in traditional data from the same system. This article describes the \IRSSquare clocking pattern and presents the equations that are needed to use \IRSSquare in systems other than NIRSpec. For NIRSpec, applying these equations is already an option in the calibration pipeline. As an aid to instrument builders, we provide our prototype \IRSSquare calibration software and sample \JWST NIRSpec data. The same techniques are applicable to other detector systems, including those based on Teledyne's H4RG arrays. The H4RG's "interleaved reference pixel readout" mode is effectively one \IRSSquare pattern.
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- 2017
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21. The Primordial Inflation Polarization Explorer (PIPER)
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Gandilo, Natalie N., Ade, Peter A. R., Benford, Dominic, Bennett, Charles L., Chuss, David T., Dotson, Jessie L., Eimer, Joseph R., Fixsen, Dale J., Halpern, Mark, Hilton, Gene, Hinshaw, Gary F., Irwin, Kent, Jhabvala, Christine, Kimball, Mark, Kogut, Alan, Lowe, Luke, McMahon, Jeff J., Miller, Timothy M., Mirel, Paul, Moseley, S. Harvey, Pawlyk, Samuel, Rodriguez, Samelys, Sharp III, Elmer, Shirron, Peter, Staguhn, Johannes G., Sullivan, Dan F., Switzer, Eric R., Taraschi, Peter, Tucker, Carole E., and Wollack, Edward J.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Primordial Inflation Polarization ExploreR (PIPER) is a balloon-borne telescope designed to measure the polarization of the Cosmic Microwave Background on large angular scales. PIPER will map 85% of the sky at 200, 270, 350, and 600 GHz over a series of 8 conventional balloon flights from the northern and southern hemispheres. The first science flight will use two 32x40 arrays of backshort-under-grid transition edge sensors, multiplexed in the time domain, and maintained at 100 mK by a Continuous Adiabatic Demagnetization Refrigerator. Front-end cryogenic Variable-delay Polarization Modulators provide systematic control by rotating linear to circular polarization at 3 Hz. Twin telescopes allow PIPER to measure Stokes I, Q, U, and V simultaneously. The telescope is maintained at 1.5 K in an LHe bucket dewar. Cold optics and the lack of a warm window permit sensitivity at the sky-background limit. The ultimate science target is a limit on the tensor-to-scalar ratio of r ~ 0.007, from the reionization bump to l ~ 300. PIPER's first flight will be from the Northern hemisphere, and overlap with the CLASS survey at lower frequencies. We describe the current status of the PIPER instrument., Comment: 8 pages, 6 figures. To be published in Proceedings of SPIE Volume 9914. Presented at SPIE Astronomical Telescopes + Instrumentation 2016, conference 9914
- Published
- 2016
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22. Detectors and cooling technology for direct spectroscopic biosignature characterization
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Rauscher, Bernard J., Canavan, Edgar R., Moseley, S. H., Sadleir, John E., and Stevenson, Thomas
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Direct spectroscopic biosignature characterization (hereafter "biosignature characterization") will be a major focus for future space observatories equipped with coronagraphs or starshades. Our aim in this article is to provide an introduction to potential detector and cooling technologies for biosignature characterization. We begin by reviewing the needs. These include nearly noiseless photon detection at flux levels as low as $<0.001~\textrm{photons}~s^{-1}~\textrm{pixel}^{-1}$ in the visible and near-IR. We then discuss potential areas for further testing and/or development to meet these needs using non-cryogenic detectors (EMCCD, HgCdTe array, HgCdTe APD array), and cryogenic single photon detectors (MKID arrays and TES microcalorimeter arrays). Non-cryogenic detectors are compatible with the passive cooling that is strongly preferred by coronagraphic missions, but would add non-negligible noise. Cryogenic detectors would require active cooling, but in return deliver nearly quantum limited performance. Based on the flight dynamics of past NASA missions, we discuss reasonable vibration expectations for a large UV-Optical-IR space telescope (LUVOIR) and preliminary cooling concepts that could potentially fit into a vibration budget without being the largest element. We believe that a cooler that meets the stringent vibration needs of a LUVOIR is also likely to meet those of a starshade-based Habitable Exoplanet Imaging Mission., Comment: 31 pages, 6 figures, and 4 tables. Submitted to the Journal of Astronomical Telescopes, Instruments, and Systems
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- 2016
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23. Far-ultraviolet Observations of Comet C/2012 S1 (ISON) from FORTIS
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McCandliss, Stephan R., Feldman, Paul D., Weaver, Harold, Fleming, Brian, Redwine, Keith, Li, Mary J., Kutyrev, Alexander, and Moseley, S. Harvey
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We have used the unique far-UV imaging capability offered by a sounding rocket borne instrument to acquire observations of C/2012 S1 (ISON) when its angular separation with respect to the sun was 26.3deg, on 2013 November 20.49. At the time of observation the comet's heliocentric distance and velocity relative to the sun were rh = 0.43 AU and rh_dot = -62.7 km s^-1. Images dominated by C I 1657 A and H I 1216 A were acquired over a 1e6 x 1e6 km^2 region. The water production rate implied by the Lyman alpha observations is constrained to be Q_H2O approximately 8e29 s^-1 while the neutral carbon production rate was Q_C approximately 4e28 s^-1. The radial profile of C I was consistent with it being a dissociation product of a parent molecule with a lifetime approximately 5e4 seconds, favoring a parent other than CO. We constrain the Q_CO production rate to 5(+1.5, -7.5)e28 s^-1 with 1sigma errors derived from photon statistics. The upper limit on the Q_CO/Q_H2O < 6%., Comment: 11 pages, 10 figures, Accepted for publication in AJ, 2016-June-17
- Published
- 2016
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24. Cosmic Infrared Background Fluctuations and Zodiacal Light
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Arendt, Richard G., Kashlinsky, A., Moseley, S. H., and Mather, J.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We have performed a specific observational test to measure the effect that the zodiacal light can have on measurements of the spatial fluctuations of the near-IR background. Previous estimates of possible fluctuations caused by zodiacal light have often been extrapolated from observations of the thermal emission at longer wavelengths and low angular resolution, or from IRAC observations of high latitude fields where zodiacal light is faint and not strongly varying with time. The new observations analyzed here target the COSMOS field, at low ecliptic latitude where the zodiacal light intensity varies by factors of $\sim2$ over the range of solar elongations at which the field can be observed. We find that the white noise component of the spatial power spectrum of the background is correlated with the modeled zodiacal light intensity. Roughly half of the measured white noise is correlated with the zodiacal light, but a more detailed interpretation of the white noise is hampered by systematic uncertainties that are evident in the zodiacal light model. At large angular scales ($\gtrsim100"$) where excess power above the white noise is observed, we find no correlation of the power with the modeled intensity of the zodiacal light. This test clearly indicates that the large scale power in the infrared background is not being caused by the zodiacal light., Comment: 17 pp. Accepted for publication in the ApJ
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- 2016
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25. A comparative study of cemented carbide parts produced by solvent on granules 3D-printing (SG-3DP) versus press and sinter
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Carreño-Morelli, E., Alveen, P., Moseley, S., Rodriguez-Arbaizar, M., and Cardoso, K.
- Published
- 2021
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26. Cosmology Large Angular Scale Surveyor (CLASS) Focal Plane Development
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Chuss, D. T., Ali, A., Amiri, M., Appel, J., Bennett, C. L., Colazo, F., Denis, K. L., Dünner, R., Essinger-Hileman, T., Eimer, J., Fluxa, P., Gothe, D., Halpern, M., Harrington, K., Hilton, G., Hinshaw, G., Hubmayr, J., Iuliano, J., Marriage, T. A., Miller, N., Moseley, S. H., Mumby, G., Petroff, M., Reintsema, C., Rostem, K., U-Yen, K., Watts, D., Wagner, E., Wollack, E. J., Xu, Z., and Zeng, L.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Cosmology Large Angular Scale Surveyor (CLASS) will measure the polarization of the Cosmic Microwave Background to search for and characterize the polarized signature of inflation. CLASS will operate from the Atacama Desert and observe $\sim$70% of the sky. A variable-delay polarization modulator (VPM) modulates the polarization at $\sim$10 Hz to suppress the 1/f noise of the atmosphere and enable the measurement of the large angular scale polarization modes. The measurement of the inflationary signal across angular scales that span both the recombination and reionization features allows a test of the predicted shape of the polarized angular power spectra in addition to a measurement of the energy scale of inflation. CLASS is an array of telescopes covering frequencies of 38, 93, 148, and 217 GHz. These frequencies straddle the foreground minimum and thus allow the extraction of foregrounds from the primordial signal. Each focal plane contains feedhorn-coupled transition-edge sensors that simultaneously detect two orthogonal linear polarizations. The use of single-crystal silicon as the dielectric for the on-chip transmission lines enables both high efficiency and uniformity in fabrication. Integrated band definition has been implemented that both controls the bandpass of the single mode transmission on the chip and prevents stray light from coupling to the detectors., Comment: 7 pages, 5 figures, accepted by the Journal of Low Temperature Physics
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- 2015
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27. Recovery of Large Angular Scale CMB Polarization for Instruments Employing Variable-delay Polarization Modulators
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Miller, N. J., Chuss, D. T., Marriage, T. A., Wollack, E. J., Appel, J. W., Bennett, C. L., Eimer, J., Essinger-Hileman, T., Fixsen, D. J., Harrington, K., Moseley, S. H., Rostem, K., Switzer, E. R., and Watts, D. J.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Variable-delay Polarization Modulators (VPMs) are currently being implemented in experiments designed to measure the polarization of the cosmic microwave background on large angular scales because of their capability for providing rapid, front-end polarization modulation and control over systematic errors. Despite the advantages provided by the VPM, it is important to identify and mitigate any time-varying effects that leak into the synchronously modulated component of the signal. In this paper, the effect of emission from a $300$ K VPM on the system performance is considered and addressed. Though instrument design can greatly reduce the influence of modulated VPM emission, some residual modulated signal is expected. VPM emission is treated in the presence of rotational misalignments and temperature variation. Simulations of time-ordered data are used to evaluate the effect of these residual errors on the power spectrum. The analysis and modeling in this paper guides experimentalists on the critical aspects of observations using VPMs as front-end modulators. By implementing the characterizations and controls as described, front-end VPM modulation can be very powerful for mitigating $1/f$ noise in large angular scale polarimetric surveys. None of the systematic errors studied fundamentally limit the detection and characterization of B-modes on large scales for a tensor-to-scalar ratio of $r=0.01$. Indeed, $r<0.01$ is achievable with commensurately improved characterizations and controls., Comment: 13 pages, 13 figures, 1 table, matches published version
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- 2015
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28. ATLAST detector needs for direct spectroscopic biosignature characterization in the visible and near-IR
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Rauscher, Bernard J., Bolcar, Matthew R., Clampin, Mark, Domagal-Goldman, Shawn D., McElwain, Michael W., Moseley, S. H., Stahle, Carl, Stark, Christopher C., and Thronson, Harley A.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Are we alone? Answering this ageless question will be a major focus for astrophysics in coming decades. Our tools will include unprecedentedly large UV-Optical-IR space telescopes working with advanced coronagraphs and starshades. Yet, these facilities will not live up to their full potential without better detectors than we have today. To inform detector development, this paper provides an overview of visible and near-IR (VISIR; $\lambda=0.4-1.8~\mu\textrm{m}$) detector needs for the Advanced Technology Large Aperture Space Telescope (ATLAST), specifically for spectroscopic characterization of atmospheric biosignature gasses. We also provide a brief status update on some promising detector technologies for meeting these needs in the context of a passively cooled ATLAST., Comment: 8 pages, Presented 9 August 2015 at SPIE Optics + Photonics, San Diego, CA
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- 2015
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29. Spectral Confusion for Cosmological Surveys of Redshifted CII Observations
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Kogut, A., Dwek, E., and Moseley, S. H.
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Astrophysics - Astrophysics of Galaxies - Abstract
Far infrared cooling lines are ubiquitous features in the spectra of star forming galaxies. Surveys of redshifted fine-structure lines provide a promising new tool to study structure formation and galactic evolution at redshifts including the epoch of reionization as well as the peak of star formation. Unlike neutral hydrogen surveys, where the 21 cm line is the only bright line, surveys of red-shifted fine-structure lines suffer from confusion generated by line broadening, spectral overlap of different lines, and the crowding of sources with redshift. We use simulations to investigate the resulting spectral confusion and derive observing parameters to minimize these effects in pencil-beam surveys of red-shifted far-IR line emission. We generate simulated spectra of the 17 brightest far-IR lines in galaxies, covering the 150 to 1300 micron wavelength region corresponding to redshifts 0 < z < 7, and develop a simple iterative algorithm that successfully identifies the 158 micron [CII] line and other lines. Although the [CII] line is a principal coolant for the interstellar medium, the assumption that the brightest observed lines in a given line of sight are always [CII] lines is a poor approximation to the simulated spectra once other lines are included. Blind line identification requires detection of fainter companion lines from the same host galaxies, driving survey sensitivity requirements. The observations require moderate spectral resolution 700 < R < 4000 with angular resolution between 20 arcsec and 10 armin, sufficiently narrow to minimize confusion yet sufficiently large to include a statistically meaningful number of sources., Comment: 7 pages including 7 figures. Accepted for publication in The Astrophysical Journal
- Published
- 2015
30. Three-dimensional printing of hard materials
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Carreño-Morelli, E., Alveen, P., Moseley, S., Rodriguez-Arbaizar, M., and Cardoso, K.
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- 2020
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31. Reconstructing emission from pre-reionization sources with cosmic infrared background fluctuation measurements by the JWST
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Kashlinsky, A., Mather, J. C., Helgason, K., Arendt, R. G., Bromm, V., and Moseley, S. H.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present new methodology to use cosmic infrared background (CIB) fluctuations to probe sources at 10
30., Comment: ApJ, in press. Minor revisions/additions to match the version in proofs - Published
- 2014
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32. The Primordial Inflation Polarization Explorer (PIPER)
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Lazear, Justin, Ade, Peter A. R., Benford, Dominic, Bennett, Charles L., Chuss, David T., Dotson, Jessie L., Eimer, Joseph R., Fixsen, Dale J., Halpern, Mark, Hilton, Gene, Hinderks, James, Hinshaw, Gary F., Irwin, Kent, Jhabvala, Christine, Johnson, Bradley, Kogut, Alan, Lowe, Luke, McMahon, Jeff J., Miller, Timothy M., Mirel, Paul, Moseley, S. Harvey, Rodriguez, Samelys, Sharp, Elmer, Staguhn, Johannes G., Switzer, Eric R., Tucker, Carole E., Weston, Amy, and Wollack, Edward J.
- Subjects
Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Primordial Inflation Polarization Explorer (PIPER) is a balloon-borne cosmic microwave background (CMB) polarimeter designed to search for evidence of inflation by measuring the large-angular scale CMB polarization signal. BICEP2 recently reported a detection of B-mode power corresponding to the tensor-to-scalar ratio r = 0.2 on ~2 degree scales. If the BICEP2 signal is caused by inflationary gravitational waves (IGWs), then there should be a corresponding increase in B-mode power on angular scales larger than 18 degrees. PIPER is currently the only suborbital instrument capable of fully testing and extending the BICEP2 results by measuring the B-mode power spectrum on angular scales $\theta$ = ~0.6 deg to 90 deg, covering both the reionization bump and recombination peak, with sensitivity to measure the tensor-to-scalar ratio down to r = 0.007, and four frequency bands to distinguish foregrounds. PIPER will accomplish this by mapping 85% of the sky in four frequency bands (200, 270, 350, 600 GHz) over a series of 8 conventional balloon flights from the northern and southern hemispheres. The instrument has background-limited sensitivity provided by fully cryogenic (1.5 K) optics focusing the sky signal onto four 32x40-pixel arrays of time-domain multiplexed Transition-Edge Sensor (TES) bolometers held at 140 mK. Polarization sensitivity and systematic control are provided by front-end Variable-delay Polarization Modulators (VPMs), which rapidly modulate only the polarized sky signal at 3 Hz and allow PIPER to instantaneously measure the full Stokes vector (I, Q, U, V) for each pointing. We describe the PIPER instrument and progress towards its first flight., Comment: 11 pages, 7 figures. To be published in Proceedings of SPIE Volume 9153. Presented at SPIE Astronomical Telescopes + Instrumentation 2014, conference 9153
- Published
- 2014
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33. The GISMO 2-millimeter Deep Field in GOODS-N
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Staguhn, Johannes G., Kovacs, Attila, Arendt, Richard G., Benford, Dominic J., Decarli, Roberto, Dwek, Eli, Fixsen, Dale J., Hilton, Gene C., Irwin, Kent D., Jhabvala, Christine A., Karim, Alexander, Leclercq, Samuel, Maher, Stephen F., Miller, Timothy M., Moseley, S. Harvey, Sharp, Elmer H., Walter, Fabian, and Wollack, Edward J.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present deep continuum observations using the GISMO camera at a wavelength of 2 mm centered on the Hubble Deep Field (HDF) in the GOODS-N field. These are the first deep field observations ever obtained at this wavelength. The 1 sigma sensitivity in the innermost approx. 4 arcminutes of the 7 utes map is approx. 135 uJy/beam, a factor of three higher in flux/beam sensitivity than the deepest available SCUBA 850 um observations, and almost a factor of four higher in flux / beam sensitivity than the combined MAMBO/AzTEC 1.2 mm observations of this region. Our source extraction algorithm identifies 12 sources directly, and another 3 through correlation with known sources at 1.2 mm and 850 um. Five of the directly detected GISMO sources have counterparts in the MAMBO/AzTEC catalog, and four of those also have SCUBA counterparts. HDF850.1, one of the first blank-field detected submillimeter galaxies, is now detected at 2 mm. The median redshift of all sources with counterparts of known redshifts is med(z) = 2.91 +/- 0.94. Statistically, the detections are most likely real for 5 of the seven 2 mm sources without shorter wavelength counterparts, while the probability for none of them being real is negligible., Comment: Accepted for publication in ApJ
- Published
- 2013
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34. Cross-correlating cosmic IR and X-ray background fluctuations: evidence of significant black hole populations among the CIB sources
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Cappelluti, N., Kashlinsky, A., Arendt, R. G., Comastri, A., Fazio, G. G., Finoguenov, A., Hasinger, G., Mather, J. C., Miyaji, T., and Moseley, S. H.
- Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
In order to understand the nature of the sources producing the recently uncovered cosmic infrared background (CIB) fluctuations, we study cross-correlations between the fluctuations in the source-subtracted CIB from Spitzer/IRAC data and the unresolved cosmic X-ray background from deep Chandra observations. Our study uses data from the EGS/AEGIS field, where both data sets cover an 8'x45' region of the sky. Our measurement is the cross-power spectrum between the IR and X-ray data. The cross-power signal between the IRAC maps at 3.6 um and 4.5 um and the Chandra [0.5-2] keV data has been detected, at angular scales 20'', with an overall significance of 3.8 sigma and 5.6 sigma, respectively. At the same time we find no evidence of significant cross-correlations at the harder Chandra bands. The cross-correlation signal is produced by individual IR sources with 3.6 um and 4.5 um magnitudes m_AB 25-26 and [0.5-2] keV X-ray fluxes 7e-17 cgs.We determine that at least 15%-25% of the large scale power of the CIB fluctuations is correlated with the spatial power spectrum of the X-ray fluctuations. If this correlation is attributed to emission from accretion processes at both IR and X-ray wavelengths, this implies a much higher fraction of accreting black holes than among the known populations. We discuss the various possible origins for the cross-power signal and show that neither local foregrounds nor the known remaining normal galaxies and active galactic nuclei can reproduce the measurements. These observational results are an important new constraint on theoretical modeling of the near-IR CIB fluctuations., Comment: 28 pages, 9 Figures, Accepted by ApJ
- Published
- 2012
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35. New measurements of the cosmic infrared background fluctuations in deep Spitzer/IRAC survey data and their cosmological implications
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Kashlinsky, A., Arendt, R. G., Ashby, M. L. N., Fazio, G. G., Mather, J., and Moseley, S. H.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We extend previous measurements of cosmic infrared background (CIB) fluctuations to ~ 1 deg using new data from the Spitzer Extended Deep Survey. Two fields, with depths of ~12 hr/pixel over 3 epochs, are analyzed at 3.6 and 4.5 mic. Maps of the fields were assembled using a self-calibration method uniquely suitable for probing faint diffuse backgrounds. Resolved sources were removed from the maps to a magnitude limit of AB mag ~ 25, as indicated by the level of the remaining shot noise. The maps were then Fourier-transformed and their power spectra were evaluated. Instrumental noise was estimated from the time-differenced data, and subtracting this isolates the spatial fluctuations of the actual sky. The power spectra of the source-subtracted fields remain identical (within the observational uncertainties) for the three epochs indicating that zodiacal light contributes negligibly to the fluctuations. Comparing to 8 mic power spectra shows that Galactic cirrus cannot account for the fluctuations. The signal appears isotropically distributed on the sky as required for an extragalactic origin. The CIB fluctuations continue to diverge to > 10 times those of known galaxy populations on angular scales out to < 1 deg. The low shot noise levels remaining in the diffuse maps indicate that the large scale fluctuations arise from the spatial clustering of faint sources well below the confusion noise. The spatial spectrum of these fluctuations is in reasonable agreement with an origin in populations clustered according to the standard cosmological model (LCDM) at epochs coinciding with the first stars era., Comment: ApJ, to be published
- Published
- 2012
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36. A superconducting dual-rail cavity qubit with erasure-detected logical measurements
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Chou, Kevin S., Shemma, Tali, McCarrick, Heather, Chien, Tzu-Chiao, Teoh, James D., Winkel, Patrick, Anderson, Amos, Chen, Jonathan, Curtis, Jacob C., de Graaf, Stijn J., Garmon, John W. O., Gudlewski, Benjamin, Kalfus, William D., Keen, Trevor, Khedkar, Nishaad, Lei, Chan U., Liu, Gangqiang, Lu, Pinlei, Lu, Yao, Maiti, Aniket, Mastalli-Kelly, Luke, Mehta, Nitish, Mundhada, Shantanu O., Narla, Anirudh, Noh, Taewan, Tsunoda, Takahiro, Xue, Sophia H., Yuan, Joseph O., Frunzio, Luigi, Aumentado, José, Puri, Shruti, Girvin, Steven M., Moseley, S. Harvey, and Schoelkopf, Robert J.
- Abstract
A critical challenge in developing scalable quantum systems is correcting the accumulation of errors while performing operations and measurements. It is known that systems where dominant errors can be detected and converted into erasures have relaxed requirements for quantum error correction. Recently, it has been proposed that this can be achieved using a dual-rail encoding of quantum information in the microwave photon states of two superconducting cavities. One necessary step to realize this erasure qubit is to demonstrate a measurement and to flag errors as erasures. In this work, we demonstrate a projective logical measurement of a dual-rail cavity qubit with integrated erasure detection and measure the qubit idling errors. We measure the logical state preparation and measurement errors at the 0.01% level and detect over 99% of the cavity decay events as erasures. We use the precision of this measurement protocol to distinguish different types of error in this system, finding that although decay errors occur with a probability of approximately 0.2% per microsecond, phase errors occur 6 times less frequently and bit flips occur at least 150 times less frequently. These findings represent a confirmation of the expected error hierarchy necessary to concatenate dual-rail cavity qubits into a highly efficient erasure code.
- Published
- 2024
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37. Properties of a Variable-delay Polarization Modulator
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Chuss, David T., Wollack, Edward J., Henry, Ross, Hui, Howard, Juarez, Aaron J., Krejny, Megan, Moseley, S. Harvey, and Novak, Giles
- Subjects
Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We investigate the polarization modulation properties of a variable-delay polarization modulator (VPM). The VPM modulates polarization via a variable separation between a polarizing grid and a parallel mirror. We find that in the limit where the wavelength is much larger than the diameter of the metal wires that comprise the grid, the phase delay derived from the geometric separation between the mirror and the grid is sufficient to characterize the device. However, outside of this range, additional parameters describing the polarizing grid geometry must be included to fully characterize the modulator response. In this paper, we report test results of a VPM at wavelengths of 350 microns and 3 mm. Electromagnetic simulations of wire grid polarizers were performed and are summarized using a simple circuit model that incorporates the loss and polarization properties of the device., Comment: 25 pages, 10 figures, accepted by Applied Optics
- Published
- 2011
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38. The Primordial Inflation Explorer (PIXIE): A Nulling Polarimeter for Cosmic Microwave Background Observations
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Kogut, A., Fixsen, D. J., Chuss, D. T., Dotson, J., Dwek, E., Halpern, M., Hinshaw, G. F., Meyer, S. M., Moseley, S. H., Seiffert, M. D., Spergel, D. N., and Wollack, E. J.
- Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Primordial Inflation Explorer (PIXIE) is an Explorer-class mission to measure the gravity-wave signature of primordial inflation through its distinctive imprint on the linear polarization of the cosmic microwave background. The instrument consists of a polarizing Michelson interferometer configured as a nulling polarimeter to measure the difference spectrum between orthogonal linear polarizations from two co-aligned beams. Either input can view the sky or a temperature-controlled absolute reference blackbody calibrator. PIXIE will map the absolute intensity and linear polarization (Stokes I, Q, and U parameters) over the full sky in 400 spectral channels spanning 2.5 decades in frequency from 30 GHz to 6 THz (1 cm to 50 um wavelength). Multi-moded optics provide background-limited sensitivity using only 4 detectors, while the highly symmetric design and multiple signal modulations provide robust rejection of potential systematic errors. The principal science goal is the detection and characterization of linear polarization from an inflationary epoch in the early universe, with tensor-to-scalar ratio r < 10^{-3} at 5 standard deviations. The rich PIXIE data set will also constrain physical processes ranging from Big Bang cosmology to the nature of the first stars to physical conditions within the interstellar medium of the Galaxy., Comment: 37 pages including 17 figures. Submitted to the Journal of Cosmology and Astroparticle Physics
- Published
- 2011
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39. The Radio - 2 mm Spectral Index of the Crab Nebula Measured with GISMO
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Arendt, R. G., George, J. V., Staguhn, J. G., Benford, D. J., Devlin, M. J., Dicker, S. R., Fixsen, D. J., Irwin, K. D., Jhabvala, C. A., Korngut, P. M., Kovács, A., Maher, S. F., Mason, B. S., Miller, T. M., Moseley, S. H., Navarro, S., Sievers, A., Sievers, J. L., Sharp, E., and Wollack, E. J.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
We present results of 2 mm observations of the Crab Nebula, obtained using the Goddard-IRAM Superconducting 2 Millimeter Observer (GISMO) bolometer camera on the IRAM 30 m telescope. Additional 3.3 mm observations with the MUSTANG bolometer array on the Green Bank Telescope are also presented. The integrated 2 mm flux density of the Crab Nebula provides no evidence for the emergence of a second synchrotron component that has been proposed. It is consistent with the radio power law spectrum, extrapolated up to a break frequency of log(nu_{b} [GHz]) = 2.84 +/- 0.29 or nu_{b} = 695^{+651}_{-336} GHz. The Crab Nebula is well-resolved by the ~16.7" beam (FWHM) of GISMO. Comparison to radio data at comparable spatial resolution enables us to confirm significant spatial variation of the spectral index between 21 cm and 2 mm. The main effect is a spectral flattening in the inner region of the Crab Nebula, correlated with the toroidal structure at the center of the nebula that is prominent in the near-IR through X-ray regime., Comment: Accepted for publication in the ApJ
- Published
- 2011
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40. On the nature of the first galaxies selected at 350 microns
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Khan, Sophia A., Chanial, Pierre F., Willner, S. P., Pearson, Chris P., Ashby, M. L. N., Benford, Dominic J., Clements, David L., Dye, Simon, Farrah, Duncan, Fazio, G. G., Huang, J. -S., Lebouteiller, V., Floc'h, Emeric Le, Mainetti, Gabriele, Moseley, S. Harvey, Negrello, Mattia, Serjeant, Stephen, Shafer, Richard A., Staguhn, Johannes, Sumner, Timothy J., and Vaccari, Mattia
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Astrophysics - Cosmology and Extragalactic Astrophysics - Abstract
[abridged] We present constraints on the nature of the first galaxies selected at 350 microns. The sample includes galaxies discovered in the deepest blank-field survey at 350 microns (in the Bootes Deep Field) and also later serendipitous detections in the Lockman Hole. Spectral energy distribution templates are fit to identified counterparts, and the sample is found to comprise IR-luminous galaxies at 1
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- 2009
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41. Cosmic Infrared Background Fluctuations in Deep Spitzer IRAC Images: Data Processing and Analysis
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Arendt, R. G., Kashlinsky, A., Moseley, S. H., and Mather, J.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
This paper provides a detailed description of the data reduction and analysis procedures that have been employed in our previous studies of spatial fluctuation of the cosmic infrared background (CIB) using deep Spitzer IRAC observations. The self-calibration we apply removes a strong instrumental signal from the fluctuations which would otherwise corrupt our results. The procedures and results for masking bright sources, and modeling faint sources down to levels set by the instrumental noise are presented. Various tests are performed to demonstrate that the resulting power spectra of these fields are not dominated by instrumental or procedural effects. These tests indicate that the large scale (>~30') fluctuations that remain in the deepest fields are not directly related to the galaxies that are bright enough to be individually detected. We provide the parameterization of these power spectra in terms of separate instrument noise, shot noise, and power law components. Our measurements of spatial fluctuations of the CIB intensity indicate the mean emission from the objects producing the fluctuations is quite low (>~1 nW m-2 sr-1 at 3-5 micron), and thus consistent with current gamma-ray absorption constraints. The source of the fluctuations may be high-z Population III objects, or a more local component of very low luminosity objects with clustering properties that differ from the resolved galaxies. Finally, we discuss the prospects of the upcoming space-based surveys to directly measure the epochs inhabited by the populations producing these source-subtracted CIB fluctuations, and to isolate the individual fluxes of these populations., Comment: 76 pages, 39 Postscript figures. Submitted to ApJS. (Abstract abridged.); 2010 ApJS, in press (Jan)
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- 2009
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42. MUSTANG: 90 GHz Science with the Green Bank Telescope
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Dicker, S. R., Korngut, P. M., Mason, B. S., Ade, P. A. R., Aguirre, J., Ames, T. J., Benford, D. J., Chen, T. C., Chervenak, J. A., Cotton, W. D., Devlin, M. J., Figueroa-Feliciano, E., Irwin, K. D., Maher, S., Mello, M., Moseley, S. H., Tally, D. J., Tucker, C., and White, S. D.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
MUSTANG is a 90 GHz bolometer camera built for use as a facility instrument on the 100 m Robert C. Byrd Green Bank radio telescope (GBT). MUSTANG has an 8 by 8 focal plane array of transition edge sensor bolometers read out using time-domain multiplexed SQUID electronics. As a continuum instrument on a large single dish MUSTANG has a combination of high resolution (8") and good sensitivity to extended emission which make it very competitive for a wide range of galactic and extragalactic science. Commissioning finished in January 2008 and some of the first science data have been collected., Comment: 9 Pages, 5 figures, Presented at the SPIE conference on astronomical instrumentation in 2008
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- 2009
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43. In Situ Probes of the First Galaxies and Reionization: Gamma-ray Bursts
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McQuinn, Matthew, Bloom, Joshua S., Grindlay, Jonathan, Band, David, Barthelmy, S. D., Berger, E., Corsi, A., Covino, S., Fishman, G. J., Furlanetto, Steven R., Gehrels, Neil, Hartmann, D. H., Kouveliotou, Chryssa, Kutyrev, A. S., Loeb, Abraham, Moseley, S. Harvey, Piran, Tsvi, Piro, L., Prochaska, J. X., Salvaterra, R., Schady, P., Soderberg, A. M., and Tagliaferri, G.
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Astrophysics - Cosmology and Extragalactic Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The first structures in the Universe formed at z>7, at higher redshift than all currently known galaxies. Since GRBs are brighter than other cosmological sources at high redshift and exhibit simple power-law afterglow spectra that is ideal for absorption studies, they serve as powerful tools for studying the early universe. New facilities planned for the coming decade will be able to obtain a large sample of high-redshift GRBs. Such a sample would constrain the nature of the first stars, galaxies, and the reionization history of the Universe., Comment: 8 pages, 3 figures, science white paper submitted to the US Astro2010 Decadal Survey
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- 2009
44. Dual-resonator kinetic inductance detector for distinction between signal and 1/f frequency noise
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Foroozani, N., primary, Sarabi, B., additional, Moseley, S. H., additional, Stevenson, T., additional, Wollack, E. J., additional, Noroozian, O., additional, and Osborn, K. D., additional
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- 2024
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45. Comparison of 3.6 - 8.0 Micron Spitzer/IRAC Galactic Center Survey Point Sources with Chandra X-Ray Point Sources in the Central 40x40 Parsecs
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Arendt, R. G., Gezari, D. Y., Stolovy, S. R., Sellgren, K., Smith, R., Ramirez, S. V., Yusef-Zadeh, F., Law, C. J., Smith, H. A., Cotera, A. S., and Moseley, S. H.
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Astrophysics - Abstract
We have studied the correlation between 2357 Chandra X-ray point sources in a 40 x 40 parsec field and ~20,000 infrared sources we observed in the corresponding subset of our 2 x 1.4 degree Spitzer/IRAC Galactic Center Survey at 3.6-8.0 um, using various spatial and X-ray hardness thresholds. The correlation was determined for source separations of less than 0.5", 1" or 2". Only the soft X-ray sources show any correlation with infrared point sources on these scales, and that correlation is very weak. The upper limit on hard X-ray sources that have infrared counterparts is <1.7% (3 sigma). However, because of the confusion limit of the IR catalog, we only detect IR sources with absolute magnitudes < ~1. As a result, a stronger correlation with fainter sources cannot be ruled out. Only one compact infrared source, IRS 13, coincides with any of the dozen prominent X-ray emission features in the 3 x 3 parsec region centered on Sgr A*, and the diffuse X-ray and infrared emission around Sgr A* seems to be anti-correlated on a few-arcsecond scale. We compare our results with previous identifications of near-infrared companions to Chandra X-ray sources., Comment: 28 pages, 8 Postscript figures (low resolution). Accepted for publication in the ApJ
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- 2008
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46. The Hertz/VPM polarimeter: Design and first light observations
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Krejny, Megan, Chuss, David, d'Aubigny, Christian Drouet, Golish, Dathon, Houde, Martin, Hui, Howard, Kulesa, Craig, Loewenstein, Robert F., Moseley, S. Harvey, Novak, Giles, Voellmer, George, Walker, Chris, and Wollack, Ed
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Astrophysics - Abstract
We present first results of Hertz/VPM, the first submillimeter polarimeter employing the dual Variable-delay Polarization Modulator (dual-VPM). This device differs from previously used polarization modulators in that it operates in translation rather than mechanical rotation. We discuss the basic theory behind this device, and its potential advantages over the commonly used half wave plate (HWP). The dual-VPM was tested both at the Submillimeter Telescope Observatory (SMTO) and in the lab. In each case we present a detailed description of the setup. We discovered nonideal behavior in the system. This is at least in part due to properties of the VPM wire grids (diameter, spacing) employed in our experiment. Despite this, we found that the dual-VPM system is robust, operating with high efficiency and low instrumental polarization. This device is well suited for air and space-borne applications., Comment: 31 pages, 11 figures, 2 tables
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- 2008
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47. Dynamical Zodiacal Cloud Models Constrained by High Resolution Spectroscopy of the Zodiacal Light (Icarus, in press)
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Ipatov, Sergei I., Kutyrev, Alexander S., Madsen, Greg J., Mather, John C., Moseley, S. Harvey, and Reynolds, Ronald J.
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Astrophysics - Abstract
The simulated Doppler shifts of the solar Mg I Fraunhofer line produced by scattering on the solar light by asteroidal, cometary, and trans-Neptunian dust particles are compared with the shifts obtained by Wisconsin H-Alpha Mapper (WHAM) spectrometer. The simulated spectra are based on the results of integrations of the orbital evolution of particles. The deviation of the derived spectral parameters for various sources of dust used in the model reached maximum at the elongation (measured eastward from the Sun) between 90 deg and 120 deg. For the future zodiacal light Doppler shifts measurements, it is important to pay a particular attention to observing at this elongation range. At the elongations of the fields observed by WHAM, the model-predicted Doppler shifts were close to each other for several scattering functions considered. Therefore the main conclusions of our paper don't depend on a scattering function and mass distribution of particles if they are reasonable. A comparison of the dependencies of the Doppler shifts on solar elongation and the mean width of the Mg I line modeled for different sources of dust with those obtained from the WHAM observations shows that the fraction of cometary particles in zodiacal dust is significant and can be dominant. Cometary particles originating inside Jupiter's orbit and particles originating beyond Jupiter's orbit (including trans-Neptunian dust particles) can contribute to zodiacal dust about 1/3 each, with a possible deviation from 1/3 up to 0.1-0.2. The fraction of asteroidal dust is estimated to be about 0.3-0.5. The mean eccentricities of zodiacal particles located at 1-2 AU from the Sun that better fit the WHAM observations are between 0.2 and 0.5, with a more probable value of about 0.3., Comment: Icarus, in press
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- 2007
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48. Demonstrating the negligible contribution of optical ACS/HST galaxies to source-subtracted cosmic infrared background fluctuations in deep IRAC/Spitzer images
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Kashlinsky, A., Arendt, R. G., Mather, J., and Moseley, S. H.
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Astrophysics - Abstract
We study the possible contribution of optical galaxies detected with the {\it Hubble} ACS instrument to the near-IR cosmic infrared (CIB) fluctuations in deep {\it Spitzer} images. The {\it Spitzer} data used in this analysis are obtained in the course of the GOODS project from which we select four independent $10^\prime\times10^\prime$ regions observed at both 3.6 and 4.5 \um. ACS source catalogs for all of these areas are used to construct maps containing only their emissions in the ACS $B, V, i, z$-bands. We find that deep Spitzer data exhibit CIB fluctuations remaining after removal of foreground galaxies of a very different clustering pattern at both 3.6 and 4.5 \um than the ACS galaxies could contribute. We also find that there are very good correlations between the ACS galaxies and the {\it removed} galaxies in the Spitzer maps, but practically no correlations remain with the residual Spitzer maps used to identify the CIB fluctuations. These contributions become negligible on larger scales used to probe the CIB fluctuations arising from clustering. This means that the ACS galaxies cannot contribute to the large-scale CIB fluctuations found in the residual Spitzer data. The absence of their contributions also means that the CIB fluctuations arise at $z\gsim 7.5$ as the Lyman break of their sources must be redshifted past the longest ACS band, or the fluctuations have to originate in the more local but extremely low luminosity galaxies., Comment: Ap.J.Letters, in press. Minor revisions to mathc the accepted version
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- 2007
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49. First Constraints on Source Counts at 350 Microns
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Khan, Sophia A., Shafer, Richard A., Serjeant, Stephen, Willner, S. P., Pearson, Chris P., Benford, Dominic J., Staguhn, Johannes G., Moseley, S. Harvey, Sumner, Timothy J., Ashby, Matthew L. N., Borys, Colin K., Chanial, Pierre, Clements, David L., Dowell, C. Darren, Dwek, Eli, Fazio, Giovanni G., Kovács, Attila, Floc'h, Emeric Le, and Silverberg, Robert F.
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Astrophysics - Abstract
We have imaged a $\sim$6 arcminute$^2$ region in the Bo\"otes Deep Field using the 350 $\mu$m-optimised second generation Submillimeter High Angular Resolution Camera (SHARC II), achieving a peak 1$\sigma$ sensitivity of $\sim$5 mJy. We detect three sources above 3$\sigma$, and determine a spurious source detection rate of 1.09 in our maps. In the absence of $5\sigma$ detections, we rely on deep 24 $\mu$m and 20 cm imaging to deduce which sources are most likely to be genuine, giving two real sources. From this we derive an integral source count of 0.84$^{+1.39}_{-0.61}$ sources arcmin$^{-2}$ at $S>13$ mJy, which is consistent with 350 $\mu$m source count models that have an IR-luminous galaxy population evolving with redshift. We use these constraints to consider the future for ground-based short-submillimetre surveys., Comment: accepted for publication in The Astrophysical Journal
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- 2007
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50. Diffraction Considerations for Planar Detectors in the Few-Mode Limit
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Chuss, David T., Wollack, Edward J., Moseley, S. Harvey, Withington, Stafford, and Saklatvala, George
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Astrophysics - Abstract
Filled arrays of bolometers are currently being employed for use in astronomy from the far-infrared through millimeter parts of the electromagnetic spectrum. Because of the large range of wavelengths for which such detectors are applicable, the number of modes supported by a pixel will vary according to the specific application of a given available technology. We study the dependence of image fidelity and induced polarization on the size of the pixel by employing a formalism in which diffraction due to the pixel boundary is treated by propagating the second-order statistical correlations of the radiation field through a model optical system. We construct polarized beam pattern images of square pixels for various ratios of p/\lambda where p is the pixel size and \lambda is the wavelength of the radiation under consideration. For the limit in which few modes are supported by the pixel (p/\lambda<1), we find that the diffraction due to the pixel edges is non-negligible and hence must be considered along with the telescope diffraction pattern in modeling the ultimate spatial resolution of an imaging system. For the case in which the pixel is over-moded (p/\lambda>1), the geometric limit is approached as expected. This technique gives a quantitative approach to optimize the imaging properties of arrays of planar detectors in the few-mode limit., Comment: 20 pages, 8 figures
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- 2007
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