Search

Your search keyword '"Shiu, Corwin"' showing total 12 results
Start Over Author "Shiu, Corwin"
12 results on '"Shiu, Corwin"'

1. Design and Performance of 30/40 GHz Diplexed Focal Plane for BICEP Array

Author

Shiu, Corwin, Soliman, Ahmed, O'Brient, Roger, Steinbach, Bryan, Bock, James J., Frez, Clifford F., Jones, William C., Megerian, Krikor G., Moncelsi, Lorenzo, Schillaci, Alessandro, Turner, Anthony D., Weber, Alexis C., Zhang, Cheng, and Zhang, Silvia

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We demonstrate a wide-band diplexed focal plane suitable for observing low-frequency foregrounds that are important for cosmic microwave background polarimetry. The antenna elements are composed of slotted bowtie antennas with 60% bandwidth that can be partitioned into two bands. Each pixel is composed of two interleaved 12$\times$12 pairs of linearly polarized antenna elements forming a phased array, designed to synthesize a symmetric beam with no need for focusing optics. The signal from each antenna element is captured in-phase and uniformly weighted by a microstrip summing tree. The antenna signal is diplexed into two bands through the use of two complementary, six-pole Butterworth filters. This filter architecture ensures a contiguous impedance match at all frequencies, and thereby achieves minimal reflection loss between both bands. Subsequently, out-of-band rejection is increased with a bandpass filter and the signal is then deposited on a transition-edge sensor bolometer island. We demonstrate the performance of this focal plane with two distinct bands, 30 and 40 GHz, each with a bandwidth of $\sim$20 and 15 GHz, respectively. The unequal bandwidths between the two bands are caused by an unintentional shift in diplexer frequency from its design values. The end-to-end optical efficiency of these detectors are relatively modest, at 20-30%, with an efficiency loss due to an unknown impedance mismatch in the summing tree. Far-field beam maps show good optical characteristics with edge pixels having no more than $\sim$ 5% ellipticity and $\sim$10-15% peak-to-peak differences for A-B polarization pairs., Comment: 17 pages, 13 figures. Accepted for publication in ApJS

Published
2024
Full Text
View/download PDF

2. Evidence for Spatial Separation of Galactic Dust Populations

Author

Shiu, Corwin, Benton, Steven J., Filippini, Jeffrey P., Fraisse, Aurélien A., Jones, William C., Nagy, Johanna M., Padilla, Ivan L., and Soler, Juan D.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an implementation of a Bayesian mixture model using Hamiltonian Monte Carlo (HMC) techniques to search for spatial separation of Galactic dust populations. Utilizing intensity measurements from Planck High Frequency Instrument (HFI), we apply this model to high-latitude Galactic dust emission. Our analysis reveals a strong preference for a spatially-varying two-population dust model over a one-population dust model, when the latter must capture the total variance in the sky. Each dust population is well characterized by a single-component spectral energy distribution (SED) and accommodates small variations. These populations could signify two distinct components, or may originate from a one-component model with different temperatures resulting in different SED scalings. While no spatial information is built into the likelihood, our investigation unveils large-scale spatially coherent structures with high significance, pointing to a physical origin for the observed spatial variation. These results are robust to our choice of likelihood and of input data. Furthermore, this spatially varying two-population model is the most favored from Bayesian evidence calculations. Incorporating IRAS 100 $\mu$m to constrain the Wein-side of the blackbody function, we find the dust populations differ at the 2.5$\sigma$ level in the spectral index ($\beta_d$) vs. temperature ($T_d$) plane. The presence of multiple dust populations has implications for component separation techniques frequently employed in the recovery of the cosmic microwave background., Comment: 19 pages, 8 figures. Accepted for publication in ApJ

Published
2023

3. Snowmass 2021 CMB-S4 White Paper

Author

Abazajian, Kevork, Abdulghafour, Arwa, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Ajello, Marco, Akerib, Daniel, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Amiri, Mandana, Anderson, Adam, Ansarinejad, Behzad, Archipley, Melanie, Arnold, Kam S., Ashby, Matt, Aung, Han, Baccigalupi, Carlo, Baker, Carina, Bakshi, Abhishek, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Barton, Paul, Thakur, Ritoban Basu, Battaglia, Nicholas, Beall, Jim, Bean, Rachel, Beck, Dominic, Belkner, Sebastian, Benabed, Karim, Bender, Amy N., Benson, Bradford A., Besuner, Bobby, Bethermin, Matthieu, Bhimani, Sanah, Bianchini, Federico, Biquard, Simon, Birdwell, Ian, Bischoff, Colin A., Bleem, Lindsey, Bocaz, Paulina, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, Francois R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chan, Victor, Chang, Clarence L., Chapman, Scott, Charles, Eric, Chauvin, Eric, Cheng, Cheng, Chesmore, Grace, Cheung, Kolen, Chinone, Yuji, Chluba, Jens, Cho, Hsiao-Mei Sherry, Choi, Steve, Clancy, Justin, Clark, Susan, Cooray, Asantha, Coppi, Gabriele, Corlett, John, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, Dai, Wei-Ming, Daley, Cail, Dart, Eli, Daues, Gregorg, de Haan, Tijmen, Deaconu, Cosmin, Delabrouille, Jacques, Derylo, Greg, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dober, Brad, Doriese, Randy, Duff, Shannon, Dutcher, Daniel, Dvorkin, Cora, Dünner, Rolando, Eftekhari, Tarraneh, Eimer, Joseph, Bouhargani, Hamza El, Elleflot, Tucker, Emerson, Nick, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Fanfani, Valentina, Fasano, Alessandro, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frisch, Josef, Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Giannakopoulos, Christos, Gilchriese, Murdock, Gluscevic, Vera, Goeckner-Wald, Neil, Goldfinger, David, Green, Daniel, Grimes, Paul, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Vic, Gudmundsson, Jon E., Gullett, Ian, Guns, Sam, Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Hand, Emma, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Herbst, Ryan, Hervias-Caimapo, Carlos, Hill, J. Colin, Hills, Richard, Hivon, Eric, Hlozek, Renée, Ho, Anna, Holder, Gil, Hollister, Matt, Holzapfel, William, Hood, John, Hotinli, Selim, Hryciuk, Alec, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, nez, Roberto Ibá, Ibitoye, Ayodeji, Ikape, Margaret, Irwin, Kent, Jacobus, Cooper, Jeong, Oliver, Johnson, Bradley R., Johnstone, Doug, Jones, William C., Joseph, John, Jost, Baptiste, Kang, Jae Hwan, Kaplan, Ari, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, King, Cesiley, Kisner, Theodore, Klein, Matthias, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Krolewski, Alex, Kubik, Donna, Kuhlmann, Steve, Kuo, Chao-Lin, Kusaka, Akito, Lähteenmäki, Anne, Lau, Kenny, Lawrence, Charles R., Lee, Adrian T., Legrand, Louis, Leitner, Matthaeus, Leloup, Clément, Lewis, Antony, Li, Dale, Linder, Eric, Liodakis, Ioannis, Liu, Jia, Long, Kevin, Louis, Thibaut, Loverde, Marilena, Lowry, Lindsay, Lu, Chunyu, Lubin, Phil, Ma, Yin-Zhe, Maccarone, Thomas, Madhavacheril, Mathew S., Maldonado, Felipe, Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, May, Jared, McCarrick, Heather, McCracken, Ken, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Miranda, Vivian, Mitchell, Don, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria Elena, Moshed, Magdy, Mroczkowski, Tony, Mukherjee, Suvodip, Münchmeyer, Moritz, Nagai, Daisuke, Nagarajappa, Chandan, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Nerval, Simran, Newburgh, Laura, Nguyen, Hogan, Nichols, Erik, Nicola, Andrina, Niemack, Michael D., Nord, Brian, Norton, Tim, Novosad, Valentine, O'Brient, Roger, Omori, Yuuki, Orlando, Giorgio, Osherson, Benjamin, Osten, Rachel, Padin, Stephen, Paine, Scott, Partridge, Bruce, Patil, Sanjaykumar, Petravick, Don, Petroff, Matthew, Pierpaoli, Elena, Pilleux, Mauricio, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Raveri, Marco, Reese, Ben, Reichardt, Christian L., Remazeilles, Mathieu, Rizzieri, Arianna, Rocha, Graca, Roe, Natalie A., Rotermund, Kaja, Roy, Anirban, Ruhl, John E., Saba, Joe, Sailer, Noah, Salatino, Maria, Saliwanchik, Benjamin, Sapozhnikov, Leonid, Rao, Mayuri Sathyanarayana, Saunders, Lauren, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Shiu, Corwin, Simon, Sara M., Singari, Baibhav, Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony A., Starkman, Glenn D., Steinbach, Bryan, Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Tandoi, Chris, Teply, Grant P., Thayer, Gregg, Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Trendafilova, Cynthia, Tristram, Matthieu, Tucker, Carole, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, van Marrewijk, Joshiwa, Vavagiakis, Eve M., Vergès, Clara, Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Wang, Guo-Jian, Watson, Scott, Watts, Duncan, Weaver, Chris, Wenzl, Lukas, Westbrook, Ben, White, Martin, Whitehorn, Nathan, Wiedlea, Andrew, Williams, Paul, Wilson, Robert, Winch, Harrison, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yefremenko, Volodymyr G., Yu, Cyndia, Zegeye, David, Zivick, Jeff, and Zonca, Andrea

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract

This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. We provide an overview of the science case, the technical design, and project plan., Comment: Contribution to Snowmass 2021. arXiv admin note: substantial text overlap with arXiv:1908.01062, arXiv:1907.04473

Published
2022

4. Probing Cosmic Reionization and Molecular Gas Growth with TIME

Author

Sun, Guochao, Chang, Tzu-Ching, Uzgil, Bade D., Bock, Jamie, Bradford, Charles M., Butler, Victoria, Caze-Cortes, Tessalie, Cheng, Yun-Ting, Cooray, Asantha, Crites, Abigail T., Hailey-Dunsheath, Steve, Emerson, Nick, Frez, Clifford, Hoscheit, Benjamin L., Hunacek, Jonathon R., Keenan, Ryan P., Li, Chao-Te, Madonia, Paolo, Marrone, Daniel P., Moncelsi, Lorenzo, Shiu, Corwin, Trumper, Isaac, Turner, Anthony, Weber, Alexis, Wei, Ta-Shun, and Zemcov, Michael

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Line intensity mapping (LIM) provides a unique and powerful means to probe cosmic structures by measuring the aggregate line emission from all galaxies across redshift. The method is complementary to conventional galaxy redshift surveys that are object-based and demand exquisite point-source sensitivity. The Tomographic Ionized-carbon Mapping Experiment (TIME) will measure the star formation rate (SFR) during cosmic reionization by observing the redshifted [CII] 158$\mu$m line ($6 \lesssim z \lesssim 9$) in the LIM regime. TIME will simultaneously study the abundance of molecular gas during the era of peak star formation by observing the rotational CO lines emitted by galaxies at $0.5 \lesssim z \lesssim 2$. We present the modeling framework that predicts the constraining power of TIME on a number of observables, including the line luminosity function, and the auto- and cross-correlation power spectra, including synergies with external galaxy tracers. Based on an optimized survey strategy and fiducial model parameters informed by existing observations, we forecast constraints on physical quantities relevant to reionization and galaxy evolution, such as the escape fraction of ionizing photons during reionization, the faint-end slope of the galaxy luminosity function at high redshift, and the cosmic molecular gas density at cosmic noon. We discuss how these constraints can advance our understanding of cosmological galaxy evolution at the two distinct cosmic epochs for TIME, starting in 2021, and how they could be improved in future phases of the experiment., Comment: 30 pages, 18 figures, accepted for publication in ApJ

Published
2020
Full Text
View/download PDF

5. Design and Performance of a 30/40 GHz Diplexed Focal Plane for the BICEP Array

Author

Shiu, Corwin, primary, Soliman, Ahmed, additional, O’Brient, Roger, additional, Steinbach, Bryan, additional, Bock, James J., additional, Frez, Clifford F., additional, Jones, William C., additional, Megerian, Krikor. G., additional, Moncelsi, Lorenzo, additional, Schillaci, Alessandro, additional, Turner, Anthony D., additional, Weber, Alexis C., additional, Zhang, Cheng, additional, and Zhang, Silvia, additional

Published
2024
Full Text
View/download PDF

6. Evidence for Spatial Separation of Galactic Dust Components

Author

Shiu, Corwin, Benton, Steven J., Jones, William C., Filippini, Jeffrey P., Fraisse, Aurélien A., Nagy, Johanna M., Padilla, Ivan L., Soler, Juan D., Shiu, Corwin, Benton, Steven J., Jones, William C., Filippini, Jeffrey P., Fraisse, Aurélien A., Nagy, Johanna M., Padilla, Ivan L., and Soler, Juan D.

Abstract

We present an implementation of a Bayesian mixture model using Hamiltonian Monte Carlo (HMC) techniques to search for spatial separation of Galactic dust components. Utilizing intensity measurements from \Planck High Frequency Instrument (HFI), we apply this model to high-latitude Galactic dust emission. Our analysis reveals a strong preference for a spatially-varying two-population dust model in intensity, with each population being well characterized by a single-component dust spectral-energy distribution (SED). While no spatial information is built into the likelihood, our investigation unveils spatially coherent structures with high significance, pointing to a physical origin for the observed spatial separation. These results are robust to our choice of likelihood and of input data. Furthermore, they are favored over a single-component dust model by Bayesian evidence calculations. Incorporating \IRAS 100\,$\mu m$ to constrain the Wein-side of the blackbody function, we find the dust populations differ at the $2.5\sigma$ level on the spectral index ($\beta_d$) vs. temperature $(T_d)$ plane. The presence of a multi-population dust has implications for component separation techniques frequently employed in the recovery of the Cosmic Microwave Background., Comment: 16 pages, 8 figures. Submitted to ApJ

Published
2023

7. SuperSpec: the on-chip spectrometer: characterization of a full 300 channel filterbank (Conference Presentation)

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Wheeler, Jordan D., Hailey-Dunsheath, Steven, Shirokoff, Erik, Barry, Peter S., Bradford, Charles M., Chapman, Scott, Che, George, Doyle, Simon, Glenn, Jason, Gordon, Samuel, Hollister, Matthew, Kovacs, Attila, LeDuc, Henry G., Mauskopf, Philip, McGeehan, Ryan, McKenney, Christopher, Reck, Theodore, Redford, Joseph, Ross, Colin, Shiu, Corwin, Tucker, Carole, Turner, Jordan, Zmuidzinas, Jonas, Gao, Jian-Rong, Wheeler, Jordan D., Hailey-Dunsheath, Steven, Shirokoff, Erik, Barry, Peter S., Bradford, Charles M., Chapman, Scott, Che, George, Doyle, Simon, Glenn, Jason, Gordon, Samuel, Hollister, Matthew, Kovacs, Attila, LeDuc, Henry G., Mauskopf, Philip, McGeehan, Ryan, McKenney, Christopher, Reck, Theodore, Redford, Joseph, Ross, Colin, Shiu, Corwin, Tucker, Carole, and Turner, Jordan

Abstract

SuperSpec is a new technology for millimeter and submillimeter spectroscopy. It is an on-chip spectrometer being developed for multi-object, moderate resolution (R = ~300), large bandwidth survey spectroscopy of high-redshift galaxies for the 1 mm atmospheric window. SuperSpec targets the CO ladder in the redshift range of z = 0 to 4, the [CII] 158 um line from z = 5 to 9, and the [NII] 205 um line from z = 4-7. All together these lines offer complete redshift coverage from z = 0 to 9. SuperSpec employs a novel architecture in which detectors are coupled to a series of resonant filters along a single microwave feedline instead of using dispersive optics. This construction allows for the creation of a full spectrometer occupying only 20 cm squared of silicon, a reduction in size of several orders of magnitude when compared to standard grating spectrometers. This small profile enables the production of future multi-object spectroscopic instruments required as the millimeter-wave spectroscopy field matures. SuperSpec uses a lens-coupled antenna to deliver astrophysical radiation to a microstrip transmission line. The radiation then propagates down this transmission line where upon proximity coupled half wavelength microstrip resonators pick off specific frequencies of radiation. Careful tuning of the proximity of the resonators to the feedline dials in the desired resolving power of the SuperSpec filterbank by tuning the coupling quality factor. The half wavelength resonators are then in turn coupled to the inductive meander of kinetic inductance detectors (KIDs), which serve as the power detectors for the SuperSpec filterbank. Each SuperSpec filter bank contains hundreds of titanium nitride TiN KIDs and the natural multiplexibility of these detectors allow for readout of the large numbers of required detectors. The unique coupling scheme employed by SuperSpec allows for the creation of incredibly low volume (2.6 cubic microns), high responsivity, TiN KIDs. Since respo

Published
2018

8. Design Considerations to Improving Sensitivity in Superspec: an Onchip KID-Based, Mm-Wave Spectrometer

Author

Shiu, Corwin, Shiu, Corwin, Shiu, Corwin, and Shiu, Corwin

Abstract

SuperSpec is an ultra-compact on-chip spectrometer for mm/submm astronomy. SuperSpec's compact size and wide spectral bandwidth will be uniquely powerful to perform multi-object spectroscopy for high redshift surveys, and for tomographic studies of the epoch of reionization (EoR). SuperSpec employs the use of kinetic inductance detectors (KID) to build highly multiplexed arrays. A full instrument of~ 500 channels can be lithographed on a few cm2 of silicon. In this thesis, we explored electromagnetic designs to improve sensitivity of KIDs. We show that we can reliably remove up to 753 of the current design's inductor volume to obtain improvements in sensitivities up a factor of four. We also explored two filter designs that can deliver higher power to the detectors. Our half-wave transmission line filters can only deliver up to 503 of power to the detectors. Both ring resonators and backshorted detectors can deliver unity power, however we found that the large coupling length needed in order to properly use ring resonators would be impractical in a. filterba.nk. Lastly we explored different filterbank designs. Multiple detectors read out together in a single channel has higher resolving power than single detector channels. Backshorted detectors offer higher resolving power than two paired detector channels, but under-performs three or more paired detector channels.

Published
2015

9. SuperSpec: the on-chip spectrometer: characterization of a full 300 channel filterbank (Conference Presentation)

Author

Wheeler, Jordan D., primary, Hailey-Dunsheath, Steven, additional, Shirokoff, Erik, additional, Barry, Peter S., additional, Bradford, Charles M., additional, Chapman, Scott, additional, Che, George, additional, Doyle, Simon M., additional, Glenn, Jason, additional, Gordon, Samuel, additional, Hollister, Matthew I., additional, Kovacs, Atilla, additional, Leduc, Henry G., additional, Mauskopf, Philip, additional, McGeehan, Ryan, additional, McKenney, Christopher M., additional, Reck, Theodore, additional, Redford, Joeseph G., additional, Ross, Colin, additional, Shiu, Corwin, additional, Tucker, Carole, additional, Turner, Jordan, additional, and Zmuidzinas, Jonas, additional

Published
2018
Full Text
View/download PDF

10. Detector modules and spectrometers for the TIME-Pilot [CII] intensity mapping experiment

Author

Hunacek, Jonathon, additional, Bock, James, additional, Bradford, C. Matt, additional, Bumble, Bruce, additional, Chang, Tzu-Ching, additional, Cheng, Yun-Ting, additional, Cooray, Asantha, additional, Crites, Abigail, additional, Hailey-Dunsheath, Steven, additional, Gong, Yan, additional, Li, Chao-Te, additional, O’Brient, Roger, additional, Shirokoff, Erik, additional, Shiu, Corwin, additional, Sun, Jason, additional, Staniszewski, Zachary, additional, Uzgil, Bade, additional, and Zemcov, Michael, additional

Published
2016
Full Text
View/download PDF

12. SuperSpec: the on-chip spectrometer: characterization of a full 300 channel filterbank (Conference Presentation)

Author

Wheeler, Jordan D., Hailey-Dunsheath, Steven, Shirokoff, Erik, Barry, Peter S., Bradford, Charles M., Chapman, Scott, Che, George, Doyle, Simon M., Glenn, Jason, Gordon, Samuel, Hollister, Matthew I., Kovacs, Atilla, Leduc, Henry G., Mauskopf, Philip, McGeehan, Ryan, McKenney, Christopher M., Reck, Theodore, Redford, Joeseph G., Ross, Colin, Shiu, Corwin, Tucker, Carole, Turner, Jordan, Zmuidzinas, Jonas, Gao, Jian-Rong, Wheeler, Jordan D., Hailey-Dunsheath, Steven, Shirokoff, Erik, Barry, Peter S., Bradford, Charles M., Chapman, Scott, Che, George, Doyle, Simon M., Glenn, Jason, Gordon, Samuel, Hollister, Matthew I., Kovacs, Atilla, Leduc, Henry G., Mauskopf, Philip, McGeehan, Ryan, McKenney, Christopher M., Reck, Theodore, Redford, Joeseph G., Ross, Colin, Shiu, Corwin, Tucker, Carole, Turner, Jordan, Zmuidzinas, Jonas, and Gao, Jian-Rong

Abstract

SuperSpec is a new technology for millimeter and submillimeter spectroscopy. It is an on-chip spectrometer being developed for multi-object, moderate resolution (R = ~300), large bandwidth survey spectroscopy of high-redshift galaxies for the 1 mm atmospheric window. SuperSpec targets the CO ladder in the redshift range of z = 0 to 4, the [CII] 158 um line from z = 5 to 9, and the [NII] 205 um line from z = 4-7. All together these lines offer complete redshift coverage from z = 0 to 9. SuperSpec employs a novel architecture in which detectors are coupled to a series of resonant filters along a single microwave feedline instead of using dispersive optics. This construction allows for the creation of a full spectrometer occupying only 20 cm squared of silicon, a reduction in size of several orders of magnitude when compared to standard grating spectrometers. This small profile enables the production of future multi-object spectroscopic instruments required as the millimeter-wave spectroscopy field matures. SuperSpec uses a lens-coupled antenna to deliver astrophysical radiation to a microstrip transmission line. The radiation then propagates down this transmission line where upon proximity coupled half wavelength microstrip resonators pick off specific frequencies of radiation. Careful tuning of the proximity of the resonators to the feedline dials in the desired resolving power of the SuperSpec filterbank by tuning the coupling quality factor. The half wavelength resonators are then in turn coupled to the inductive meander of kinetic inductance detectors (KIDs), which serve as the power detectors for the SuperSpec filterbank. Each SuperSpec filter bank contains hundreds of titanium nitride TiN KIDs and the natural multiplexibility of these detectors allow for readout of the large numbers of required detectors. The unique coupling scheme employed by SuperSpec allows for the creation of incredibly low volume (2.6 cubic microns), high responsivity, TiN KIDs. Since respo

Catalog

Books, media, physical & digital resources
See catalog results