Dan Marrone

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Scholarly Contributions

Journals/Publications

• Collaboration, E., & al., e. (2021). First M87 Event Horizon Telescope Results. VII. Polarization of the Ring. Astrophysical Journal Letters, 910(1), L12.
• Collaboration, E., & al., e. (2021). First M87 Event Horizon Telescope Results. VIII. Magnetic Field Structure near The Event Horizon. Astrophysical Journal Letters, 910(1), L13.
• Goddi, C., & al., e. (2021). Polarimetric Properties of Event Horizon Telescope Targets from ALMA. Astrophysical Journal Letters, 910(1), L14.
• Group, E., & al., e. (2021). Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign. Astrophysical Journal Letters, 911(1), L11.
• Guns, S., Foster, A., Daley, C., Rahlin, A., Whitehorn, N., Ade, P., Ahmed, Z., Anderes, E., Anderson, A., Archipley, M., Avva, J., Aylor, K., Balkenhol, L., Barry, P., Basu Thakur, R., Benabed, K., Bender, A., Benson, B., Bianchini, F., , Bleem, L., et al. (2021). Detection of Galactic and Extragalactic Millimeter-wavelength Transient Sources with SPT-3G. Astrophysical Journal, 916(2), 98.
• Issaoun, S., Johnson, M., Blackburn, L., Broderick, A., Tiede, P., Wielgus, M., Doeleman, S., Falcke, H., Akiyama, K., Bower, G., Brinkerink, C., Chael, A., Cho, I., G{\'omez}, J., Hern{\'andez-G\'omez}, A., Hughes, D., Kino, M., Krichbaum, T., Liuzzo, E., , Loinard, L., et al. (2021). Persistent Non-Gaussian Structure in the Image of Sagittarius A* at 86 GHz. Astrophysical Journal, 915(2), 99.
• Janssen, M., & al., e. (2021). Event Horizon Telescope observations of the jet launching and collimation in Centaurus A. Nature Astronomy, 5, 1017-1028.
• Jarugula, S., Vieira, J. D., Weiss, A., Spilker, J. S., Aravena, M., Archipley, M., B{\'ethermin}, M., Chapman, S. C., Dong, C., Greve, T. R., Harrington, K., Hayward, C. C., Hezaveh, Y., Hill, R., Litke, K. C., Malkan, M. A., Marrone, D. P., Narayanan, D., Phadke, K. A., , Reuter, C., et al. (2021). Molecular Line Observations in Two Dusty Star-forming Galaxies at z = 6.9. Astrophysical Journal, 921(1), 97.
• Kocherlakota, P., & al., e. (2021). Constraints on black-hole charges with the 2017 EHT observations of M87*. Physical Review D, 103(10), 104047.
• Narayan, R., & al., e. (2021). The Polarized Image of a Synchrotron-emitting Ring of Gas Orbiting a Black Hole. Astrophysical Journal, 912(1), 35.
• Rotermund, K., Chapman, S., Phadke, K., Hill, R., Pass, E., Aravena, M., Ashby, M., Babul, A., B{\'ethermin}, M., Canning, R., Breuck, C., Dong, C., Gonzalez, A., Hayward, C., Jarugula, S., Marrone, D., Narayanan, D., Reuter, C., Scott, D., , Spilker, J., et al. (2021). Optical and near-infrared observations of the SPT2349-56 proto-cluster core at z = 4.3. Monthly Notices of the Royal Astronomical Society, 502(2), 1797-1815.
• Sun, G., Chang, T. -., Uzgil, B., Bock, J., Bradford, C., Butler, V., Caze-Cortes, T. .., Cheng, Y. -., Cooray, A., Crites, A., Hailey-Dunsheath, S. .., Emerson, N., Frez, C., Hoscheit, B., Hunacek, J., Keenan, R., Li, C., Madonia, P., Marrone, D., , Moncelsi, L., et al. (2021). Probing Cosmic Reionization and Molecular Gas Growth with TIME. Astrophysical Journal, 915(1), 33.
• Wang, G. C., Hill, R., Chapman, S., Wei{\ss}, A., Scott, D., Apostolovski, Y., Aravena, M., Archipley, M. A., B{\'ethermin}, M., Canning, R., De, B. C., Dong, C., Everett, W., Gonzalez, A., Greve, T. R., Hayward, C. C., Hezaveh, Y., Jarugula, S., Marrone, D., , Phadke, K. A., et al. (2021). Overdensities of submillimetre-bright sources around candidate protocluster cores selected from the South Pole Telescope survey. Monthly Notices of the Royal Astronomical Society, 508(3), 3754-3770.
• Yue, M., Yang, J., Fan, X., Wang, F., Spilker, J., Georgiev, I. Y., Keeton, C. R., Litke, K. C., Marrone, D. P., Walter, F., Wang, R., Wu, X., Venemans, B. P., & Zabludoff, A. (2021). ALMA Observations of the Sub-kpc Structure of the Host Galaxy of a z = 6.5 Lensed Quasar: A Rotationally Supported Hyper-Starburst System at the Epoch of Reionization. Astrophysical Journal, 917(2), 99.
• Cunningham, D., Chapman, S., Aravena, M., De Breuck, C., B{\'ethermin}, M., Chen, C., Dong, C., Gonzalez, A., Greve, T., Litke, K., Ma, J., Malkan, M., Marrone, D., Miller, T., Phadke, K., Reuter, C., Rotermund, K., Spilker, J., Stark, A., , Strandet, M., et al. (2020). The [C II]/[N II] ratio in 3 < z < 6 sub-millimetre galaxies from the South Pole Telescope survey. Monthly Notices of the Royal Astronomical Society, 494(3), 4090-4097.
• Everett, W., Zhang, L., Crawford, T., Vieira, J., Aravena, M., Archipley, M., Austermann, J., Benson, B., Bleem, L., Carlstrom, J., Chang, C., Chapman, S., Crites, A., Haan, T., Dobbs, M., George, E., Halverson, N., Harrington, N., Holder, G., , Holzapfel, W., et al. (2020). Millimeter-wave Point Sources from the 2500 Square Degree SPT-SZ Survey: Catalog and Population Statistics. Astrophysical Journal, 900(1), 55.
• Gold, R., & al., e. (2020). Verification of Radiative Transfer Schemes for the EHT. Astrophysical Journal, 897(2), 148.
• Gralla, S. E., Lupsasca, A., & Marrone, D. P. (2020). The shape of the black hole photon ring: A precise test of strong-field general relativity. Physical Review D, 102(12), 124004.
• Hill, R., Chapman, S., Scott, D., Apostolovski, Y., Aravena, M., B{\'ethermin}, M., Bradford, C., Canning, R. E., De, B. C., Dong, C., Gonzalez, A., Greve, T. R., Hayward, C. C., Hezaveh, Y., Litke, K., Malkan, M., Marrone, D. P., Phadke, K., Reuter, C., , Rotermund, K., et al. (2020). Megaparsec-scale structure around the protocluster core SPT2349-56 at z = 4.3. Monthly Notices of the Royal Astronomical Society, 495(3), 3124-3159.
• Keating, G. K., Marrone, D. P., Bower, G. C., & Keenan, R. P. (2020). An Intensity Mapping Detection of Aggregate CO Line Emission at 3 mm. Astrophysical Journal, 901(2), 141.
• Keenan, R. P., Marrone, D. P., & Keating, G. K. (2020). Biases and Cosmic Variance in Molecular Gas Abundance Measurements at High Redshift. Astrophysical Journal, 904(2), 127.
• Kim, J., & al., e. (2020). Event Horizon Telescope imaging of the archetypal blazar 3C 279 at an extreme 20 microarcsecond resolution. Astronomy & Astrophysics, 640, A69.
• Psaltis}, D.,
• Reuter, C., Vieira, J., Spilker, J., Weiss, A., Aravena, M., Archipley, M., B{\'ethermin}, M., Chapman, S., De Breuck, C., Dong, C., Everett, W., Fu, J., Greve, T., Hayward, C., Hill, R., Hezaveh, Y., Jarugula, S., Litke, K., Malkan, M., , Marrone, D., et al. (2020). The Complete Redshift Distribution of Dusty Star-forming Galaxies from the SPT-SZ Survey. Astrophysical Journal, 902(1), 78.
• Roelofs, F., & al., e. (2020). SYMBA: An end-to-end VLBI synthetic data generation pipeline. Simulating Event Horizon Telescope observations of M 87. Astronomy & Astrophysics, 636, A5.
• Spilker, J. S., Aravena, M., Phadke, K. A., B{\'ethermin}, M., Chapman, S. C., Dong, C., Gonzalez, A. H., Hayward, C. C., Hezaveh, Y. D., Litke, K. C., Malkan, M. A., Marrone, D. P., Narayanan, D., Reuter, C., Vieira, J. D., & Wei{\ss}, A. (2020). Ubiquitous Molecular Outflows in z > 4 Massive, Dusty Galaxies. II. Momentum-driven Winds Powered by Star Formation in the Early Universe. Astrophysical Journal, 905(2), 86.
• Spilker, J. S., Phadke, K. A., Aravena, M., B{\'ethermin}, M., Chapman, S. C., Dong, C., Gonzalez, A. H., Hayward, C. C., Hezaveh, Y. D., Jarugula, S., Litke, K. C., Malkan, M. A., Marrone, D. P., Narayanan, D., Reuter, C., Vieira, J. D., & Weiss, A. (2020). Ubiquitous Molecular Outflows in z > 4 Massive, Dusty Galaxies. I. Sample Overview and Clumpy Structure in Molecular Outflows on 500 pc Scales. Astrophysical Journal, 905(2), 85.
• Wielgus, M., & al., e. (2020). Monitoring the Morphology of M87* in 2009-2017 with the Event Horizon Telescope. Astrophysical Journal, 901(1), 67.
• Abbott}, T., Abdalla, F., Alarcon, A., Allam, S., Annis, J., Avila, S., Aylor, K., Banerji, M., Banik, N., Baxter, E., Bechtol, K., Becker, M., Benson, B., Bernstein, G., Bertin, E., Bianchini, F., Blazek, J., Bleem, L., Bridle, S., , Brooks, D., et al. (2019). Dark Energy Survey year 1 results: Joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions. Physical Review D, 100(2), 023541.
• Abdulla, Z., Carlstrom, J. E., Mantz, A. B., Marrone, D. P., Greer, C. H., Lamb, J. W., Leitch, E. M., Muchovej, S., O'Donnell, C., Plagge, T. J., & Woody, D. (2019). Constraints on the Thermal Contents of the X-Ray Cavities of Cluster MS 0735.6+7421 with Sunyaev-Zel'dovich Effect Observations. Astrophysical Journal, 871(2), 195.
• Apostolovski, Y., Aravena, M., Anguita, T., Spilker, J., Wei{\ss}, A., B{\'ethermin}, M., Chapman, S. C., Chen, C., Cunningham, D., De, B. C., Dong, C., Hayward, C. C., Hezaveh, Y., Jarugula, S., Litke, K., Ma, J., Marrone, D. P., Narayanan, D., Reuter, C. A., , Rotermund, K., et al. (2019). Imaging the molecular interstellar medium in a gravitationally lensed star-forming galaxy at z = 5.7. Astronomy & Astrophysics, 628, A23.
• Bocquet, S., Dietrich, J., Schrabback, T., Bleem, L., Klein, M., Allen, S., Applegate, D., Ashby, M., Bautz, M., Bayliss, M., Benson, B., Brodwin, M., Bulbul, E., Canning, R., Capasso, R., Carlstrom, J., Chang, C., Chiu, I., Cho, H. -., , Clocchiatti, A., et al. (2019). Cluster Cosmology Constraints from the 2500 deg^2 SPT-SZ Survey: Inclusion of Weak Gravitational Lensing Data from Magellan and the Hubble Space Telescope. Astrophysical Journal, 878(1), 55.
• Bower, G. C., Dexter, J., Asada, K., Brinkerink, C. D., Falcke, H., Ho, P., Inoue, M., Markoff, S., Marrone, D. P., Matsushita, S., Moscibrodzka, M., Nakamura, M., Peck, A., & Rao, R. (2019). ALMA Observations of the Terahertz Spectrum of Sagittarius A*. Astrophysical Journal Letters, 881(1), L2.
• Decker, B., Brodwin, M., Abdulla, Z., Gonzalez, A. H., Marrone, D. P., O'Donnell, C., Stanford, S., Wylezalek, D., Carlstrom, J. E., Eisenhardt, P. R., Mantz, A., Mo, W., Moravec, E., Stern, D., Aldering, G., Ashby, M. L., Boone, K., Hayden, B., Gupta, N., & McDonald, M. A. (2019). The Massive and Distant Clusters of WISE Survey. VI. Stellar Mass Fractions of a Sample of High-redshift Infrared-selected Clusters. Astrophysical Journal, 878(1), 72.
• Dietrich, J., Bocquet, S., Schrabback, T., Applegate, D., Hoekstra, H., Grandis, S., Mohr, J., Allen, S., Bayliss, M., Benson, B., Bleem, L., Brodwin, M., Bulbul, E., Capasso, R., Chiu, I., Crawford, T., Gonzalez, A., Haan, T., Klein, M., , Linden, A., et al. (2019). Sunyaev-Zel'dovich effect and X-ray scaling relations from weak lensing mass calibration of 32 South Pole Telescope selected galaxy clusters. Monthly Notices of the Royal Astronomical Society, 483(3), 2871-2906.
• Dong, C., Spilker, J. S., Gonzalez, A. H., Apostolovski, Y., Aravena, M., B{\'ethermin}, M., Chapman, S. C., Chen, C., Hayward, C. C., Hezaveh, Y. D., Litke, K. C., Ma, J., Marrone, D. P., Morningstar, W. R., Phadke, K. A., Reuter, C. A., Sreevani, J., Stark, A. A., Vieira, J. D., & Wei{\ss}, A. (2019). Source Structure and Molecular Gas Properties from High-resolution CO Imaging of SPT-selected Dusty Star-forming Galaxies. Astrophysical Journal, 873(1), 50.
• Farahi, A., Mulroy, S. L., Evrard, A. E., Smith, G. P., Finoguenov, A., Bourdin, H., Carlstrom, J. E., Haines, C. P., Marrone, D. P., Martino, R., Mazzotta, P., O'Donnell, C., & Okabe, N. (2019). Detection of anti-correlation of hot and cold baryons in galaxy clusters. Nature Communications, 10, 2504.
• Gonzalez, A. H., Gettings, D. P., Brodwin, M., Eisenhardt, P. R., Stanford, S., Wylezalek, D., Decker, B., Marrone, D. P., Moravec, E., O'Donnell, C., Stalder, B., Stern, D., Abdulla, Z., Brown, G., Carlstrom, J., Chambers, K. C., Hayden, B., Lin, Y., Magnier, E., , Masci, F. J., et al. (2019). The Massive and Distant Clusters of WISE Survey. I. Survey Overview and a Catalog of >2000 Galaxy Clusters at z ~ 1. Astrophysical Journal Supplement, 240(2), 33.
• Gupta, N., Reichardt, C., Ade, P., Anderson, A., Archipley, M., Austermann, J., Avva, J., Beall, J., Bender, A., Benson, B., Bianchini, F., Bleem, L., Carlstrom, J., Chang, C., Chiang, H., Citron, R., Moran, C. C., Crawford, T., Crites, A., , Haan, T., et al. (2019). Fractional polarization of extragalactic sources in the 500 deg^2 SPTpol survey. Monthly Notices of the Royal Astronomical Society, 490(4), 5712-5721.
• Horizon Telescope Collaboration, E. (2019). First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole. Astrophysical Journal Letters, 875(1), L1.
• Horizon Telescope Collaboration, E. (2019). First M87 Event Horizon Telescope Results. II. Array and Instrumentation. Astrophysical Journal Letters, 875(1), L2.
• Horizon Telescope Collaboration, E. (2019). First M87 Event Horizon Telescope Results. III. Data Processing and Calibration. Astrophysical Journal Letters, 875(1), L3.
• Horizon Telescope Collaboration, E. (2019). First M87 Event Horizon Telescope Results. IV. Imaging the Central Supermassive Black Hole. Astrophysical Journal Letters, 875(1), L4.
• Horizon Telescope Collaboration, E. (2019). First M87 Event Horizon Telescope Results. V. Physical Origin of the Asymmetric Ring. Astrophysical Journal Letters, 875(1), L5.
• Issaoun, S., Johnson, M., Blackburn, L., Brinkerink, C., Mo{\'scibrodzka}, M., Chael, A., Goddi, C., Mart{\'\i-Vidal}, I., Wagner, J., Doeleman, S., Falcke, H., Krichbaum, T., Akiyama, K., Bach, U., Bouman, K., Bower, G., Broderick, A., Cho, I., Crew, G., , Dexter, J., et al. (2019). The Size, Shape, and Scattering of Sagittarius A* at 86 GHz: First VLBI with ALMA. Astrophysical Journal, 871(1), 30.
• Litke, K. C., Marrone, D. P., Spilker, J. S., Aravena, M., B{\'ethermin}, M., Chapman, S., Chen, C., Breuck, C., Dong, C., Gonzalez, A., Greve, T. R., Hayward, C. C., Hezaveh, Y., Jarugula, S., Ma, J., Morningstar, W., Narayanan, D., Phadke, K., Reuter, C., , Vieira, J., et al. (2019). Spatially Resolved [C II] Emission in SPT0346-52: A Hyper-starburst Galaxy Merger at z = 5.7. Astrophysical Journal, 870(2), 80.
• Mocanu, L., Crawford, T., Aylor, K., Benson, B., Bleem, L., Carlstrom, J., Chang, C., Cho, H. -., Chown, R., Crites, A., Haan, T., Dobbs, M., Everett, W., George, E., Halverson, N., Harrington, N., Henning, J., Holder, G., Holzapfel, W., , Hou, Z., et al. (2019). Consistency of cosmic microwave background temperature measurements in three frequency bands in the 2500-square-degree SPT-SZ survey. Journal of Cosmology and Astroparticle Physics, 2019(7), 038.
• Mulroy, S. L., Farahi, A., Evrard, A. E., Smith, G. P., Finoguenov, A., O'Donnell, C., Marrone, D. P., Abdulla, Z., Bourdin, H., Carlstrom, J. E., D{\'emocl\`es}, J., Haines, C. P., Martino, R., Mazzotta, P., McGee, S. L., & Okabe, N. (2019). LoCuSS: scaling relations between galaxy cluster mass, gas, and stellar content. Monthly Notices of the Royal Astronomical Society, 484(1), 60-80.
• Omori}, Y., Baxter, E., Chang, C., Kirk, D., Alarcon, A., Bernstein, G., Bleem, L., Cawthon, R., Choi, A., Chown, R., Crawford, T., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T., Fosalba, P., Friedrich, O., Gatti, M., , Gaztanaga, E., et al. (2019). Dark Energy Survey Year 1 Results: Cross-correlation between Dark Energy Survey Y1 galaxy weak lensing and South Pole Telescope+Planck CMB weak lensing. Physical Review D, 100(4), 043517.
• Omori}, Y., Giannantonio, T., Porredon, A., Baxter, E., Chang, C., Crocce, M., Fosalba, P., Alarcon, A., Banik, N., Blazek, J., Bleem, L., Bridle, S., Cawthon, R., Choi, A., Chown, R., Crawford, T., Dodelson, S., Drlica-Wagner, A. .., Eifler, T., , Elvin-Poole, J. .., et al. (2019). Dark Energy Survey Year 1 Results: Tomographic cross-correlations between Dark Energy Survey galaxies and CMB lensing from South Pole Telescope +Planck. Physical Review D, 100(4), 043501.
• Porth, O., & al., e. (2019). The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project. Astrophysical Journal Supplement, 243(2), 26.
• Prat}, J., Baxter, E., Shin, T., S{\'anchez}, C., Chang, C., Jain, B., Miquel, R., Alarcon, A., Bacon, D., Bernstein, G., Cawthon, R., Crawford, T., Davis, C., De Vicente, J., Dodelson, S., Eifler, T., Friedrich, O., Gatti, M., Gruen, D., , Hartley, W., et al. (2019). Cosmological lensing ratios with DES Y1, SPT, and Planck. Monthly Notices of the Royal Astronomical Society, 487(1), 1363-1379.
• Telescope Collaboration, E. H. (2019). First M87 Event Horizon Telescope Results. VI. The Shadow and Mass of the Central Black Hole. Astrophysical Journal Letters, 875(1), L6.
• Trumper, I., Marrone, D. P., & Kim, D. W. (2019). Utilizing freeform optics in dynamic optical configuration designs. Journal of Astronomical Telescopes, Instruments, and Systems, 5, 035005.
• Viero, M., Reichardt, C., Benson, B., Bleem, L., Bock, J., Carlstrom, J., Chang, C., Cho, H. -., Crawford, T., Crites, A., Haan, T., Dobbs, M., Everett, W., George, E., Halverson, N., Harrington, N., Holder, G., Holzapfel, W., Hou, Z., , Hrubes, J., et al. (2019). Measurements of the Cross-spectra of the Cosmic Infrared and Microwave Backgrounds from 95 to 1200 GHz. Astrophysical Journal, 881(2), 96.
• Baxter, E., Raghunathan, S., Crawford, T., Fosalba, P., Hou, Z., Holder, G., Omori, Y., Patil, S., Rozo, E., Abbott, T., Annis, J., Aylor, K., Benoit-L{\'evy}, A., Benson, B., Bertin, E., Bleem, L., Buckley-Geer, E. .., Burke, D., Carlstrom, J., , Carnero Rosell, A., et al. (2018). A measurement of CMB cluster lensing with SPT and DES year 1 data. Monthly Notices of the Royal Astronomical Society, 476, 2674-2688.
• Bower, G., Broderick, A., Dexter, J., Doeleman, S., Falcke, H., Fish, V., Johnson, M., Marrone, D., Moran, J., Moscibrodzka, M., Peck, A., Plambeck, R., & Rao, R. (2018). ALMA Polarimetry of Sgr A*: Probing the Accretion Flow from the Event Horizon to the Bondi Radius. Astrophysical Journal, 868, 101.
• B{\'ethermin}, M., Greve, T., De Breuck, C., Vieira, J., Aravena, M., Chapman, S., Chen, C., Dong, C., Hayward, C., Hezaveh, Y., Marrone, D., Narayanan, D., Phadke, K., Reuter, C., Spilker, J., Stark, A., Strandet, M., & Wei{\ss}, A. (2018). Dense-gas tracers and carbon isotopes in five 2.5 < z < 4 lensed dusty star-forming galaxies from the SPT SMG sample. Astronomy & Astrophysics, 620, A115.
• Chown}, R., Omori, Y., Aylor, K., Benson, B., Bleem, L., Carlstrom, J., Chang, C., Cho, H., Crawford, T., Crites, A., Haan, T., Dobbs, M., Everett, W., George, E., Henning, J., Halverson, N., Harrington, N., Holder, G., Holzapfel, W., , Hou, Z., et al. (2018). Maps of the Southern Millimeter-wave Sky from Combined 2500 deg$^2$ SPT-SZ and Planck Temperature Data. Astrophysical Journal Supplement, 239, 10.
• Fazio, G., Hora, J., Witzel, G., Willner, S., Ashby, M., Baganoff, F., Becklin, E., Carey, S., Haggard, D., Gammie, C., Ghez, A., Gurwell, M., Ingalls, J., Marrone, D., Morris, M., & Smith, H. (2018). Multiwavelength Light Curves of Two Remarkable Sagittarius A* Flares. Astrophysical Journal, 864, 58.
• Hou, Z., Aylor, K., Benson, B., Bleem, L., Carlstrom, J., Chang, C., Cho, H., Chown, R., Crawford, T., Crites, A., Haan, T., Dobbs, M., Everett, W., Follin, B., George, E., Halverson, N., Harrington, N., Holder, G., Holzapfel, W., , Hrubes, J., et al. (2018). A Comparison of Maps and Power Spectra Determined from South Pole Telescope and Planck Data. Astrophysical Journal, 853, 3.
• Hunacek, J., Bock, J., Bradford, C., Butler, V., Chang, T., Cheng, Y., Cooray, A., Crites, A., Frez, C., Hailey-Dunsheath, S. .., Hoscheit, B., Kim, D., Li, C., Marrone, D., Moncelsi, L., Shirokoff, E., Steinbach, B., Sun, G., Trumper, I., , Turner, A., et al. (2018). Hafnium Films and Magnetic Shielding for TIME, A mm-Wavelength Spectrometer Array. Journal of Low Temperature Physics, 193, 893-900.
• Kim, J., Marrone, D., Roy, A., Wagner, J., Asada, K., Beaudoin, C., Blanchard, J., Carlstrom, J., Chen, M., Crawford, T., Crew, G., Doeleman, S., Fish, V., Greer, C., Gurwell, M., Henning, J., Inoue, M., Keisler, R., Krichbaum, T., , Lu, R., et al. (2018). The 1.4 mm Core of Centaurus A: First VLBI Results with the South Pole Telescope. Astrophysical Journal, 861, 129.
• Lu, R., Krichbaum, T., Roy, A., Fish, V., Doeleman, S., Johnson, M., Akiyama, K., Psaltis, D., Alef, W., Asada, K., Beaudoin, C., Bertarini, A., Blackburn, L., Blundell, R., Bower, G., Brinkerink, C., Broderick, A., Cappallo, R., Crew, G., , Dexter, J., et al. (2018). Detection of Intrinsic Source Structure at ~3 Schwarzschild Radii with Millimeter-VLBI Observations of SAGITTARIUS A*. Astrophysical Journal, 859, 60.
• Mantz, A., Abdulla, Z., Allen, S., Carlstrom, J., Logan, C., Marrone, D., Maughan, B., Willis, J., Pacaud, F., & Pierre, M. (2018). The XXL Survey. XVII. X-ray and Sunyaev-Zel'dovich properties of the redshift 2.0 galaxy cluster XLSSC 122. Astronomy & Astrophysics, 620, A2.
• Marrone, D., Spilker, J., Hayward, C., Vieira, J., Aravena, M., Ashby, M., Bayliss, M., B{\'ethermin}, M., Brodwin, M., Bothwell, M., Carlstrom, J., Chapman, S., Chen, C., Crawford, T., Cunningham, D., De Breuck, C., Fassnacht, C., Gonzalez, A., Greve, T., , Hezaveh, Y., et al. (2018). Galaxy growth in a massive halo in the first billion years of cosmic history. Nature, 553, 51-54.
• Medeiros, L., Chan, C., {\"Ozel}, F., Psaltis, D., Kim, J., Marrone, D., & Sa{\c, d. A. (2018). GRMHD Simulations of Visibility Amplitude Variability for Event Horizon Telescope Images of Sgr A*. Astrophysical Journal, 856, 163.
• Miller, T., Chapman, S., Aravena, M., Ashby, M., Hayward, C., Vieira, J., Wei{\ss}, A., Babul, A., B{\'ethermin}, M., Bradford, C., Brodwin, M., Carlstrom, J., Chen, C., Cunningham, D., De Breuck, C., Gonzalez, A., Greve, T., Harnett, J., Hezaveh, Y., , Lacaille, K., et al. (2018). A massive core for a cluster of galaxies at a redshift of 4.3. Nature, 556, 469-472.
• Spilker, J., Aravena, M., B{\'ethermin}, M., Chapman, S., Chen, C., Cunningham, D., De Breuck, C., Dong, C., Gonzalez, A., Hayward, C., Hezaveh, Y., Litke, K., Ma, J., Malkan, M., Marrone, D., Miller, T., Morningstar, W., Narayanan, D., Phadke, K., , Sreevani, J., et al. (2018). Fast molecular outflow from a dusty star-forming galaxy in the early Universe. Science, 361, 1016-1019.
• Aylor, K., Hou, Z., Knox, L., Story, K., Benson, B., Bleem, L., Carlstrom, J., Chang, C., Cho, H., Chown, R., Crawford, T., Crites, A., Haan, T., Dobbs, M., Everett, W., George, E., Halverson, N., Harrington, N., Holder, G., , Holzapfel, W., et al. (2017). A Comparison of Cosmological Parameters Determined from CMB Temperature Power Spectra from the South Pole Telescope and the Planck Satellite. Astrophysical Journal, 850, 101.
• Bothwell, M., Aguirre, J., Aravena, M., Bethermin, M., Bisbas, T., Chapman, S., De Breuck, C., Gonzalez, A., Greve, T., Hezaveh, Y., Ma, J., Malkan, M., Marrone, D., Murphy, E., Spilker, J., Strandet, M., Vieira, J., & Wei{\ss}, A. (2017). ALMA observations of atomic carbon in z~4 dusty star-forming galaxies. Monthly Notices of the Royal Astronomical Society, 466, 2825-2841.
• Mantz, A., Abdulla, Z., Allen, S., Carlstrom, J., Logan, C., Marrone, D., Maughan, B., Willis, J., Pacaud, F., & Pierre, M. (2017). The XXL Survey: XVII. X-ray and Sunyaev-Zel'dovich Properties of the Redshift 2.0 Galaxy Cluster XLSSC 122. Astronomy & Astrophysics (Accepted, awaiting XXL special issue).
• Medeiros, L., Chan, C., {\"Ozel}, F., Psaltis, D., Kim, J., Marrone, D., & Sa{\c, d. A. (2017). Variability in GRMHD Simulations of Sgr A*: Implications for EHT Closure Phase Observations. Astrophysical Journal, 844, 35.
• Omori, Y., Chown, R., Simard, G., Story, K., Aylor, K., Baxter, E., Benson, B., Bleem, L., Carlstrom, J., Chang, C., Cho, H., Crawford, T., Crites, A., Haan, T., Dobbs, M., Everett, W., George, E., Halverson, N., Harrington, N., , Holder, G., et al. (2017). A 2500 deg^2 CMB Lensing Map from Combined South Pole Telescope and Planck Data. Astrophysical Journal, 849, 124.
• Russell, H., McDonald, M., McNamara, B., Fabian, A., Nulsen, P., Bayliss, M., Benson, B., Brodwin, M., Carlstrom, J., Edge, A., Hlavacek-Larrondo, J. .., Marrone, D., Reichardt, C., & Vieira, J. (2017). Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster. Astrophysical Journal, 836, 130.
• Strandet, M., Weiss, A., De Breuck, C., Marrone, D., Vieira, J., Aravena, M., Ashby, M., B{\'ethermin}, M., Bothwell, M., Bradford, C., Carlstrom, J., Chapman, S., Cunningham, D., Chen, C., Fassnacht, C., Gonzalez, A., Greve, T., Gullberg, B., Hayward, C., , Hezaveh, Y., et al. (2017). ISM Properties of a Massive Dusty Star-forming Galaxy Discovered at z ~ 7. Astrophysical Journal Letters, 842, L15.
• Aravena, M., Spilker, J., Bethermin, M., Bothwell, M., Chapman, S., Breuck, C., Furstenau, R., G{\'onzalez-L\'opez}, J., Greve, T., Litke, K., Ma, J., Malkan, M., Marrone, D., Murphy, E., Stark, A., Strandet, M., Vieira, J., Weiss, A., Welikala, N., , Wong, G., et al. (2016). A survey of the cold molecular gas in gravitationally lensed star-forming galaxies at z $\gt$ 2. Monthly Notices of the Royal Astronomical Society, 457, 4406-4420.
• Bally, J., Blake, G., Bolatto, A., Casey, C., Church, S., Francesco, J., Goldsmith, P., Goodman, A., Harris, A., Jackson, J., Leroy, A., Lockman, F., Lovell, A., Marscher, A., Marrone, D., Mason, B., Mroczkowski, T., Shirley, Y., & Yun, M. (2016). The Case for a Publicly Available, Well-Instrumented GBT Operating at 20-115 GHz. ArXiv e-prints.
• Bayliss, M., Ruel, J., Stubbs, C., Allen, S., Applegate, D., Ashby, M., Bautz, M., Benson, B., Bleem, L., Bocquet, S., Brodwin, M., Capasso, R., Carlstrom, J., Chang, C., Chiu, I., Cho, H., Clocchiatti, A., Crawford, T., Crites, A., , Haan, T., et al. (2016). SPT-GMOS: A Gemini/GMOS-South Spectroscopic Survey of Galaxy Clusters in the SPT-SZ Survey. Astrophysical Journal Supplement, 227, 3.
• B{\'ethermin}, M., De Breuck, C., Gullberg, B., Aravena, M., Bothwell, M., Chapman, S., Gonzalez, A., Greve, T., Litke, K., Ma, J., Malkan, M., Marrone, D., Murphy, E., Spilker, J., Stark, A., Strandet, M., Vieira, J., Wei{\ss}, A., & Welikala, N. (2016). An ALMA view of the interstellar medium of the z = 4.77 lensed starburst SPT-S J213242-5802.9. Astronomy & Astrophysics, 586, L7.
• Crawford, T., Chown, R., Holder, G., Aird, K., Benson, B., Bleem, L., Carlstrom, J., Chang, C., Cho, H., Crites, A., Haan, T., Dobbs, M., George, E., Halverson, N., Harrington, N., Holzapfel, W., Hou, Z., Hrubes, J., Keisler, R., , Knox, L., et al. (2016). Maps of the Magellanic Clouds from Combined South Pole Telescope and PLANCK Data. Astrophysical Journal Supplement, 227, 23.
• Fish, V., Johnson, M., Doeleman, S., Broderick, A., Psaltis, D., Lu, R., Akiyama, K., Alef, W., Algaba, J., Asada, K., Beaudoin, C., Bertarini, A., Blackburn, L., Blundell, R., Bower, G., Brinkerink, C., Cappallo, R., Chael, A., Chamberlin, R., , Chan, C., et al. (2016). Persistent Asymmetric Structure of Sagittarius A* on Event Horizon Scales. Astrophysical Journal, 820, 90.
• Haan, T., Benson, B., Bleem, L., Allen, S., Applegate, D., Ashby, M., Bautz, M., Bayliss, M., Bocquet, S., Brodwin, M., Carlstrom, J., Chang, C., Chiu, I., Cho, H., Clocchiatti, A., Crawford, T., Crites, A., Desai, S., Dietrich, J., , Dobbs, M., et al. (2016). Cosmological Constraints from Galaxy Clusters in the 2500 Square-degree SPT-SZ Survey. Astrophysical Journal, 832, 95.
• Hezaveh, Y., Dalal, N., Marrone, D., Mao, Y., Morningstar, W., Wen, D., Blandford, R., Carlstrom, J., Fassnacht, C., Holder, G., Kemball, A., Marshall, P., Murray, N., Perreault Levasseur, L., Vieira, J., & Wechsler, R. (2016). Detection of Lensing Substructure Using ALMA Observations of the Dusty Galaxy SDP.81. Astrophysical Journal, 823, 37.
• Keating, G., Marrone, D., Bower, G., Leitch, E., Carlstrom, J., & DeBoer, D. (2016). COPSS II: The Molecular Gas Content of Ten Million Cubic Megaparsecs at Redshift z \tilde 3. Astrophysical Journal, 830, 34.
• Kim, J., Marrone, D., Chan, C., Medeiros, L., {\"Ozel}, F., & Psaltis, D. (2016). Bayesian Techniques for Comparing Time-dependent GRMHD Simulations to Variable Event Horizon Telescope Observations. Astrophysical Journal, 832, 156.
• Ma, J., Gonzalez, A., Vieira, J., Aravena, M., Ashby, M., B{\'ethermin}, M., Bothwell, M., Brandt, W., Breuck, C., Carlstrom, J., Chapman, S., Gullberg, B., Hezaveh, Y., Litke, K., Malkan, M., Marrone, D., McDonald, M., Murphy, E., Spilker, J., , Sreevani, J., et al. (2016). SPT0346-52: Negligible AGN Activity in a Compact, Hyper-starburst Galaxy at z = 5.7. Astrophysical Journal, 832, 114.
• Mo, W., Gonzalez, A., Jee, M., Massey, R., Rhodes, J., Brodwin, M., Eisenhardt, P., Marrone, D., Stanford, S., & Zeimann, G. (2016). IDCS J1426.5+3508: Weak Lensing Analysis of a Massive Galaxy Cluster at z = 1.75. Astrophysical Journal Letters, 818, L25.
• Spilker, J., Bezanson, R., Marrone, D., Weiner, B., Whitaker, K., & Williams, C. (2016). Low Gas Fractions Connect Compact Star-forming Galaxies to Their z \~{} 2 Quiescent Descendants. Astrophysical Journal, 832, 19.
• Spilker, J., Marrone, D., Aravena, M., B{\'ethermin}, M., Bothwell, M., Carlstrom, J., Chapman, S., Crawford, T., Breuck, C., Fassnacht, C., Gonzalez, A., Greve, T., Hezaveh, Y., Litke, K., Ma, J., Malkan, M., Rotermund, K., Strandet, M., Vieira, J., , Weiss, A., et al. (2016). ALMA Imaging and Gravitational Lens Models of South Pole Telescope\mdashSelected Dusty, Star-Forming Galaxies at High Redshifts. Astrophysical Journal, 826, 112.
• Stone, J., Marrone, D., Dowell, C., Schulz, B., Heinke, C., & Yusef-Zadeh, F. .. (2016). Far Infrared Variability of Sagittarius A*: 25.5 hr of Monitoring with Herschel. Astrophysical Journal, 825, 32.
• Strandet, M., Weiss, A., Vieira, J., Breuck, C., Aguirre, J., Aravena, M., Ashby, M., B{\'ethermin}, M., Bradford, C., Carlstrom, J., Chapman, S., Crawford, T., Everett, W., Fassnacht, C., Furstenau, R., Gonzalez, A., Greve, T., Gullberg, B., Hezaveh, Y., , Kamenetzky, J., et al. (2016). The Redshift Distribution of Dusty Star-forming Galaxies from the SPT Survey. Astrophysical Journal, 822, 80.
• {McDonald}, M., {Stalder}, B., {Bayliss}, M., {Allen}, S., {Applegate}, D., {Ashby}, M., {Bautz}, M., {Benson}, B., {Bleem}, L., {Brodwin}, M., {Carlstrom}, J., {Chiu}, I., {Desai}, S., {Gonzalez}, A., {Hlavacek-Larrondo}, J., {Holzapfel}, W., {Marrone}, D., {Miller}, E., {Reichardt}, C., , {Saliwanchik}, B., et al. (2016). Star-forming Brightest Cluster Galaxies at 0.25 $\gt$ z $\gt$ 1.25: A Transitioning Fuel Supply. Astrophysical Journal, 817, 86.
• {Smith}, G., {Mazzotta}, P., {Okabe}, N., {Ziparo}, F., {Mulroy}, S., {Babul}, A., {Finoguenov}, A., {McCarthy}, I., {Lieu}, M., {Bah{\'e}}, Y., {Bourdin}, H., {Evrard}, A., {Futamase}, T., {Haines}, C., {Jauzac}, M., {Marrone}, D., {Martino}, R., {May}, P., {Taylor}, J., , K. (2016). LoCuSS: Testing hydrostatic equilibrium in galaxy clusters. Monthly Notices of the Royal Astronomical Society, 456, L74-L78.
• {Welikala}, N., {B{\'e}thermin}, M., {Guery}, D., {Strandet}, M., {Aird}, K., {Aravena}, M., {Ashby}, M., {Bothwell}, M., {Beelen}, A., {Bleem}, L., {de Breuck}, C., {Brodwin}, M., {Carlstrom}, J., {Chapman}, S., {Crawford}, T., {Dole}, H., {Dor{\'e}}, O., {Everett}, W., {Flores-Cacho}, I., , {Gonzalez}, A., et al. (2016). Probing star formation in the dense environments of z {\tilde} 1 lensing haloes aligned with dusty star-forming galaxies detected with the South Pole Telescope. Monthly Notices of the Royal Astronomical Society, 455, 1629-1646.
• {Zauderer}, B., {Bolatto}, A., {Vogel}, S., {Carpenter}, J., {Per{\'e}z}, L., {Lamb}, J., {Woody}, D., {Bock}, D., {Carlstrom}, J., {Culverhouse}, T., {Curley}, R., {Leitch}, E., {Plambeck}, R., {Pound}, M., {Marrone}, D., {Muchovej}, S., {Mundy}, L., {Teng}, S., {Teuben}, P., , {Volgenau}, N., et al. (2016). The CARMA Paired Antenna Calibration System: Atmospheric Phase Correction for Millimeter Wave Interferometry and Its Application to Mapping the Ultraluminous Galaxy Arp 193. Astronomical Journal, 151, 18.
• Sharon}, K., {Gladders}, M., {Marrone}, D., {Hoekstra}, H., {Rasia}, E., {Bourdin}, H., {Gifford}, D., {Hicks}, A., {Greer}, C., {Mroczkowski}, T., {Barrientos}, L., {Bayliss}, M., {Carlstrom}, J., {Gilbank}, D., {Gralla}, M., {Hlavacek-Larrondo}, J., {Leitch}, E., {Mazzotta}, P., {Miller}, C., , {Muchovej}, S., et al. (2015). A Multi-wavelength Mass Analysis of RCS2 J232727.6-020437, A {\tilde}3 {\times} 10$^{15}$ M$_{⊙}$ Galaxy Cluster at z = 0.7. Astrophysical Journal, 814, 21.
• {Akiyama}, K., {Lu}, R., {Fish}, V., {Doeleman}, S., {Broderick}, A., {Dexter}, J., {Hada}, K., {Kino}, M., {Nagai}, H., {Honma}, M., {Johnson}, M., {Algaba}, J., {Asada}, K., {Brinkerink}, C., {Blundell}, R., {Bower}, G., {Cappallo}, R., {Crew}, G., {Dexter}, M., , {Dzib}, S., et al. (2015). 230 GHz VLBI Observations of M87: Event-horizon-scale Structure during an Enhanced Very-high-energy {$\gamma$}-Ray State in 2012. Astrophysical Journal, 807, 150.
• {Baxter}, E., {Keisler}, R., {Dodelson}, S., {Aird}, K., {Allen}, S., {Ashby}, M., {Bautz}, M., {Bayliss}, M., {Benson}, B., {Bleem}, L., {Bocquet}, S., {Brodwin}, M., {Carlstrom}, J., {Chang}, C., {Chiu}, I., {Cho}, H., {Clocchiatti}, A., {Crawford}, T., {Crites}, A., , {Desai}, S., et al. (2015). A Measurement of Gravitational Lensing of the Cosmic Microwave Background by Galaxy Clusters Using Data from the South Pole Telescope. Astrophysical Journal, 806, 247.
• {Bleem}, L., {Stalder}, B., {de Haan}, T., {Aird}, K., {Allen}, S., {Applegate}, D., {Ashby}, M., {Bautz}, M., {Bayliss}, M., {Benson}, B., {Bocquet}, S., {Brodwin}, M., {Carlstrom}, J., {Chang}, C., {Chiu}, I., {Cho}, H., {Clocchiatti}, A., {Crawford}, T., {Crites}, A., , {Desai}, S., et al. (2015). Galaxy Clusters Discovered via the Sunyaev-Zel'dovich Effect in the 2500-Square-Degree SPT-SZ Survey. Astrophysical Journal Supplement, 216, 27.
• {Bocquet}, S., {Saro}, A., {Mohr}, J., {Aird}, K., {Ashby}, M., {Bautz}, M., {Bayliss}, M., {Bazin}, G., {Benson}, B., {Bleem}, L., {Brodwin}, M., {Carlstrom}, J., {Chang}, C., {Chiu}, I., {Cho}, H., {Clocchiatti}, A., {Crawford}, T., {Crites}, A., {Desai}, S., , {de Haan}, T., et al. (2015). Mass Calibration and Cosmological Analysis of the SPT-SZ Galaxy Cluster Sample Using Velocity Dispersion {$\sigma$}$_{ v }$ and X-Ray Y $_{X}$ Measurements. Astrophysical Journal, 799, 214.
• {Bower}, G., {Demorest}, P., {Braatz}, J., {Broderick}, A., {Burke-Spolaor}, S., {Butler}, B., {Chang}, T., {Chomiuk}, L., {Cordes}, J., {Darling}, J., {Eilek}, J., {Hallinan}, G., {Kanekar}, N., {Kramer}, M., {Marrone}, D., {Max-Moerbeck}, W., {Metzger}, B., {Morales}, M., {Myers}, S., , {Osten}, R., et al. (2015). Next Generation Very Large Array Memo No. 9 Science Working Group 4: Time Domain, Fundamental Physics, and Cosmology. Next Generation Very Large Array Memo.
• {Bower}, G., {Markoff}, S., {Dexter}, J., {Gurwell}, M., {Moran}, J., {Brunthaler}, A., {Falcke}, H., {Fragile}, P., {Maitra}, D., {Marrone}, D., {Peck}, A., {Rushton}, A., , M. (2015). Radio and Millimeter Monitoring of Sgr A*: Spectrum, Variability, and Constraints on the G2 Encounter. Astrophysical Journal, 802, 69.
• {Brodwin}, M., {Greer}, C., {Leitch}, E., {Stanford}, S., {Gonzalez}, A., {Gettings}, D., {Abdulla}, Z., {Carlstrom}, J., {Decker}, B., {Eisenhardt}, P., {Lin}, H., {Mantz}, A., {Marrone}, D., {McDonald}, M., {Stalder}, B., {Stern}, D., , D. (2015). The Massive and Distant Clusters of WISE Survey. III. Sunyaev-Zel'dovich Masses of Galaxy Clusters at z{\tilde}1. Astrophysical Journal, 806, 26.
• {Buddendiek}, A., {Schrabback}, T., {Greer}, C., {Hoekstra}, H., {Sommer}, M., {Eifler}, T., {Erben}, T., {Erler}, J., {Hicks}, A., {High}, F., {Hildebrandt}, H., {Marrone}, D., {Morris}, R., {Muzzin}, A., {Reiprich}, T., {Schirmer}, M., {Schneider}, P., & Linden}, A. (2015). Optical and Sunyaev-Zel'dovich observations of a new sample of distant rich galaxy clusters in the ROSAT All Sky. Monthly Notices of the Royal Astronomical Society, 450, 4248-4276.
• {Chan}, C., {Psaltis}, D., {{\"O}zel}, F., {Medeiros}, L., {Marrone}, D., {Sa{\c d}owski}, A., , R. (2015). Fast Variability and Millimeter/IR Flares in GRMHD Models of Sgr A* from Strong-field Gravitational Lensing. Astrophysical Journal, 812, 103.
• {Gonzalez}, A., {Decker}, B., {Brodwin}, M., {Eisenhardt}, P., {Marrone}, D., {Stanford}, S., {Stern}, D., {Wylezalek}, D., {Aldering}, G., {Abdulla}, Z., {Boone}, K., {Carlstrom}, J., {Fagrelius}, P., {Gettings}, D., {Greer}, C., {Hayden}, B., {Leitch}, E., {Lin}, Y., {Mantz}, A., , {Muchovej}, S., et al. (2015). The Massive and Distant Clusters of WISE Survey: MOO J1142+1527, a 10$^{15}$ M$_{⊙}$ Galaxy Cluster at z = 1.19. Astrophysical Journal Letters, 812, L40.
• {Gullberg}, B., {De Breuck}, C., {Vieira}, J., {Wei{\ss}}, A., {Aguirre}, J., {Aravena}, M., {B{\'e}thermin}, M., {Bradford}, C., {Bothwell}, M., {Carlstrom}, J., {Chapman}, S., {Fassnacht}, C., {Gonzalez}, A., {Greve}, T., {Hezaveh}, Y., {Holzapfel}, W., {Husband}, K., {Ma}, J., {Malkan}, M., , {Marrone}, D., et al. (2015). The nature of the [C II] emission in dusty star-forming galaxies from the SPT survey. Monthly Notices of the Royal Astronomical Society, 449, 2883-2900.
• {Johnson}, M., {Fish}, V., {Doeleman}, S., {Marrone}, D., {Plambeck}, R., {Wardle}, J., {Akiyama}, K., {Asada}, K., {Beaudoin}, C., {Blackburn}, L., {Blundell}, R., {Bower}, G., {Brinkerink}, C., {Broderick}, A., {Cappallo}, R., {Chael}, A., {Crew}, G., {Dexter}, J., {Dexter}, M., , {Freund}, R., et al. (2015). Resolved magnetic-field structure and variability near the event horizon of Sagittarius A*. Science, 350, 1242-1245.
• {Keating}, G., {Bower}, G., {Marrone}, D., {DeBoer}, D., {Heiles}, C., {Chang}, T., {Carlstrom}, J., {Greer}, C., {Hawkins}, D., {Lamb}, J., {Leitch}, E., {Miller}, A., {Muchovej}, S., , D. (2015). First Results from COPSS: The CO Power Spectrum Survey. Astrophysical Journal, 814, 140.
• {Keisler}, R., {Hoover}, S., {Harrington}, N., {Henning}, J., {Ade}, P., {Aird}, K., {Austermann}, J., {Beall}, J., {Bender}, A., {Benson}, B., {Bleem}, L., {Carlstrom}, J., {Chang}, C., {Chiang}, H., {Cho}, H., {Citron}, R., {Crawford}, T., {Crites}, A., {de Haan}, T., , {Dobbs}, M., et al. (2015). Measurements of Sub-degree B-mode Polarization in the Cosmic Microwave Background from 100 Square Degrees of SPTpol Data. Astrophysical Journal, 807, 151.
• {Ma}, J., {Gonzalez}, A., {Spilker}, J., {Strandet}, M., {Ashby}, M., {Aravena}, M., {B{\'e}thermin}, M., {Bothwell}, M., {de Breuck}, C., {Brodwin}, M., {Chapman}, S., {Fassnacht}, C., {Greve}, T., {Gullberg}, B., {Hezaveh}, Y., {Malkan}, M., {Marrone}, D., {Saliwanchik}, B., {Vieira}, J., , {Weiss}, A., et al. (2015). Stellar Masses and Star Formation Rates of Lensed, Dusty, Star-forming Galaxies from the SPT Survey. Astrophysical Journal, 812, 88.
• {Psaltis}, D., {{\"O}zel}, F., {Chan}, C., , D. (2015). A General Relativistic Null Hypothesis Test with Event Horizon Telescope Observations of the Black Hole Shadow in Sgr A*. Astrophysical Journal, 814, 115.
• {Saliwanchik}, B., {Montroy}, T., {Aird}, K., {Bayliss}, M., {Benson}, B., {Bleem}, L., {Bocquet}, S., {Brodwin}, M., {Carlstrom}, J., {Chang}, C., {Cho}, H., {Clocchiatti}, A., {Crawford}, T., {Crites}, A., {de Haan}, T., {Desai}, S., {Dobbs}, M., {Dudley}, J., {Foley}, R., , {Forman}, W., et al. (2015). Measurement of Galaxy Cluster Integrated Comptonization and Mass Scaling Relations with the South Pole Telescope. Astrophysical Journal, 799, 137.
• {Spilker}, J., {Aravena}, M., {Marrone}, D., {B{\'e}thermin}, M., {Bothwell}, M., {Carlstrom}, J., {Chapman}, S., {Collier}, J., {de Breuck}, C., {Fassnacht}, C., {Galvin}, T., {Gonzalez}, A., {Gonz{\'a}lez-L{\'o}pez}, J., {Grieve}, K., {Hezaveh}, Y., {Ma}, J., {Malkan}, M., {O'Brien}, A., {Rotermund}, K., , {Strandet}, M., et al. (2015). Sub-kiloparsec Imaging of Cool Molecular Gas in Two Strongly Lensed Dusty, Star-forming Galaxies. Astrophysical Journal, 811, 124.
• {Wagner}, J., {Roy}, A., {Krichbaum}, T., {Alef}, W., {Bansod}, A., {Bertarini}, A., {G{\"u}sten}, R., {Graham}, D., {Hodgson}, J., {M{\"a}rtens}, R., {Menten}, K., {Muders}, D., {Rottmann}, H., {Tuccari}, G., {Weiss}, A., {Wieching}, G., {Wunderlich}, M., {Zensus}, J., {Araneda}, J., , {Arriagada}, O., et al. (2015). First 230 GHz VLBI fringes on 3C 279 using the APEX Telescope. Astronomy & Astrophysics, 581, A32.
• Ashby, M. L., Stanford, S. A., Brodwin, M., Gonzalez, A. H., Martinez-Manso, J., Bartlett, J. G., Benson, B. A., Bleem, L. E., Crawford, T. M., Dey, A., Dressler, A., Eisenhardt, P. R., Galametz, A., Jannuzi, B. T., Marrone, D. P., Mei, S., Muzzin, A., Pacaud, F., Pierre, M., , Stern, D., et al. (2014). Erratum: ''The Spitzer South Pole Telescope Deep Field: Survey Design and Infrared Array Camera Catalogs'' (2013, ApJS, 209, 22). Astrophysical Journal Supplement, 212, 16.
• Bayliss, M. B., Ashby, M. L., Ruel, J., Brodwin, M., Aird, K. A., Bautz, M. W., Benson, B. A., Bleem, L. E., Bocquet, S., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., Desai, S., Dobbs, M. A., Dudley, J. P., Foley, R. J., , Forman, W. R., et al. (2014). SPT-CL J2040-4451: An SZ-selected Galaxy Cluster at z = 1.478 with Significant Ongoing Star Formation. Astrophysical Journal, 794, 12.
• Dexter, J., Kelly, B., Bower, G. C., Marrone, D. P., Stone, J., & Plambeck, R. (2014). An 8 h characteristic time-scale in submillimetre light curves of Sagittarius A*. Monthly Notices of the Royal Astronomical Society, 442, 2797-2808.
• Hull, C. L., Plambeck, R. L., Kwon, W., Bower, G. C., Carpenter, J. M., Crutcher, R. M., Fiege, J. D., Franzmann, E., Hakobian, N. S., Heiles, C., Houde, M., Hughes, A. M., Lamb, J. W., Looney, L. W., Marrone, D. P., Matthews, B. C., Pillai, T., Pound, M. W., Rahman, N., , Sandell, G., et al. (2014). TADPOL: A 1.3 mm Survey of Dust Polarization in Star-forming Cores and Regions. Astrophysical Journal Supplement, 213, 13.
• Johnson, M. D., Fish, V. L., Doeleman, S. S., Broderick, A. E., Wardle, J. F., & Marrone, D. P. (2014). Relative Astrometry of Compact Flaring Structures in Sgr A* with Polarimetric Very Long Baseline Interferometry. Astrophysical Journal, 794, 150.
• Mantz, A. B., Abdulla, Z., Carlstrom, J. E., Greer, C. H., Leitch, E. M., Marrone, D. P., Muchovej, S., Adami, C., Birkinshaw, M., Bremer, M., Clerc, N., Giles, P., Horellou, C., Maughan, B., Pacaud, F., Pierre, M., & Willis, J. (2014). The XXL Survey. V. Detection of the Sunyaev-Zel'dovich Effect of the Redshift 1.9 Galaxy Cluster XLSSU J021744.1-034536 with CARMA. Astrophysical Journal, 794, 157.
• Martino, R., Mazzotta, P., Bourdin, H., Smith, G. P., Bartalucci, I., Marrone, D. P., Finoguenov, A., & Okabe, N. (2014). LoCuSS: hydrostatic mass measurements of the high-L$_X$ cluster sample - cross-calibration of Chandra and XMM-Newton. Monthly Notices of the Royal Astronomical Society, 443, 2342-2360.
• McDonald, M., Benson, B. A., Vikhlinin, A., Aird, K. A., Allen, S. W., Bautz, M., Bayliss, M., Bleem, L. E., Bocquet, S., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., Haan, T., Dobbs, M. A., Foley, R. J., , Forman, W. R., et al. (2014). The Redshift Evolution of the Mean Temperature, Pressure, and Entropy Profiles in 80 SPT-Selected Galaxy Clusters. Astrophysical Journal, 794, 67.
• McDonald, M., Swinbank, M., Edge, A. C., Wilner, D. J., Veilleux, S., Benson, B. A., Hogan, M. T., Marrone, D. P., McNamara, B. R., Wei, L. H., Bayliss, M. B., & Bautz, M. W. (2014). The state of the warm and cold gas in the extreme starburst at the core of the phoenix galaxy cluster (SPT-CLJ2344-4243). Astrophysical Journal, 784(1).
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  Abstract: We present new optical integral field spectroscopy (Gemini South) and submillimeter spectroscopy (Submillimeter Array) of the central galaxy in the Phoenix cluster (SPT-CLJ2344-4243). This cluster was previously reported to have a massive starburst (∼800 M yr-1) in the central, brightest cluster galaxy, most likely fueled by the rapidly cooling intracluster medium. These new data reveal a complex emission-line nebula, extending for >30 kpc from the central galaxy, detected at [O II]λλ3726, 3729, [O III]λλ4959, 5007, Hβ, Hγ, Hδ, [Ne III]λ3869, and He II λ4686. The total Hα luminosity, assuming Hα/Hβ = 2.85, is L Hα = 7.6 ± 0.4 ×1043 erg s-1, making this the most luminous emission-line nebula detected in the center of a cool core cluster. Overall, the relative fluxes of the low-ionization lines (e.g., [O II], Hβ) to the UV continuum are consistent with photoionization by young stars. In both the center of the galaxy and in a newly discovered highly ionized plume to the north of the galaxy, the ionization ratios are consistent with both shocks and active galactic nucleus (AGN) photoionization. We speculate that this extended plume may be a galactic wind, driven and partially photoionized by both the starburst and central AGN. Throughout the cluster we measure elevated high-ionization line ratios (e.g., He II/Hβ, [O III]/Hβ), coupled with an overall high-velocity width (FWHM ≳ 500 km s-1), suggesting that shocks are likely important throughout the interstellar medium of the central galaxy. These shocks are most likely driven by a combination of stellar winds from massive young stars, core-collapse supernovae, and the central AGN. In addition to the warm, ionized gas, we detect a substantial amount of cold, molecular gas via the CO(3-2) transition, coincident in position with the galaxy center. We infer a molecular gas mass of = 2.2 ± 0.6 × 1010 M, which implies that the starburst will consume its fuel in ∼30 Myr if it is not replenished. The L IR/ that we measure for this cluster is consistent with the starburst limit of 500 L/M, above which radiation pressure is able to disperse the cold reservoir. The combination of the high level of turbulence in the warm phase and the high L IR/ ratio suggests that this violent starburst may be in the process of quenching itself. We propose that phases of rapid star formation may be common in the cores of galaxy clusters, but so short-lived that their signatures are quickly erased and appear only in a subsample of the most strongly cooling clusters. © 2014. The American Astronomical Society. All rights reserved.
• Messias, H., Dye, S., Nagar, N., Orellana, G., Bussmann, R. S., Calanog, J., Dannerbauer, H., Fu, H., Ibar, E., Inohara, A., Ivison, R. J., Negrello, M., Riechers, D. A., Sheen, Y., Aguirre, J. E., Amber, S., Birkinshaw, M., Bourne, N., Bradford, C. M., , Clements, D. L., et al. (2014). Herschel-ATLAS and ALMA. HATLAS J142935.3-002836, a lensed major merger at redshift 1.027. Astronomy & Astrophysics, 568, A92.
• Mulroy, S. L., Smith, G. P., Haines, C. P., Marrone, D. P., Okabe, N., Pereira, M. J., Egami, E., Babul, A., Finoguenov, A., & Martino, R. (2014). LoCuSS: the near-infrared luminosity and weak-lensing mass scaling relation of galaxy clusters. Monthly Notices of the Royal Astronomical Society, 443, 3309-3317.
• Plambeck, R. L., Bower, G. C., Rao, R., Marrone, D. P., Jorstad, S. G., Marscher, A. P., Doeleman, S. S., Fish, V. L., & Johnson, M. D. (2014). Probing the Parsec-scale Accretion Flow of 3C 84 with Millimeter Wavelength Polarimetry. Astrophysical Journal, 797, 66.
• Rao, R., Girart, J. M., Lai, S., & Marrone, D. P. (2014). Detection of a magnetized disk around a very young protostar. Astrophysical Journal Letters, 780(1).
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  Abstract: We present subarcsecond resolution polarimetric observations of the 878 μm thermal dust continuum emission obtained with the Submillimeter Array toward the IRAS 16293-2422 protostellar binary system. We report the detection of linearly polarized dust emission arising from the circumstellar disk associated with the IRAS 16293-2422 B protostar. The fractional polarization of ≃ 1.4% is only slightly lower than that expected from theoretical calculations in such disks. The magnetic field structure on the plane of the sky derived from the dust polarization suggests a complex magnetic field geometry in the disk, possibly associated with a rotating disk that is wrapping the field lines as expected from the simulations. The polarization around IRAS 16293-2422 A at subarcsecond angular resolution is only marginally detected. © 2014. The American Astronomical Society. All rights reserved..
• Ruel, J., Bazin, G., Bayliss, M., Brodwin, M., Foley, R. J., Stalder, B., Aird, K. A., Armstrong, R., Ashby, M. L., Bautz, M., Benson, B. A., Bleem, L. E., Bocquet, S., Carlstrom, J. E., Chang, C. L., Chapman, S. C., Cho, H. M., Clocchiatti, A., Crawford, T. M., , Crites, A. T., et al. (2014). Optical Spectroscopy and Velocity Dispersions of Galaxy Clusters from the SPT-SZ Survey. Astrophysical Journal, 792, 45.
• Saro, A., Liu, J., Mohr, J. J., Aird, K. A., Ashby, M. L., Bayliss, M., Benson, B. A., Bleem, L. E., Bocquet, S., Brodwin, M., Carlstrom, J. E., Chang, C. L., Chiu, I., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., Haan, T., Desai, S., , Dietrich, J. P., et al. (2014). Constraints on the CMB temperature evolution using multiband measurements of the Sunyaev-Zel'dovich effect with the South Pole Telescope. Monthly Notices of the Royal Astronomical Society, 440, 2610-2615.
• Spilker, J. S., Marrone, D. P., Aguirre, J. E., Aravena, M., Ashby, M. L., B'ethermin, M., Bradford, C. M., Bothwell, M. S., Brodwin, M., Carlstrom, J. E., Chapman, S. C., Crawford, T. M., Breuck, C., Fassnacht, C. D., Gonzalez, A. H., Greve, T. R., Gullberg, B., Hezaveh, Y., Holzapfel, W. L., , Husband, K., et al. (2014). The Rest-frame Submillimeter Spectrum of High-redshift, Dusty, Star-forming Galaxies. Astrophysical Journal, 785, 149.
• Aravena, M., Murphy, E. J., Aguirre, J. E., Ashby, M. L., Benson, B. A., Bothwell, M., Brodwin, M., Carlstrom, J. E., Chapman, S. C., Crawford, T. M., C., d. B., Fassnacht, C. D., Gonzalez, A. H., Greve, T. R., Gullberg, B., Hezaveh, Y., Holder, G. P., Holzapfel, W. L., Keisler, R., , Malkan, M., et al. (2013). Large gas reservoirs and free-free emission in two lensed star-forming galaxies at z = 2.7. Monthly Notices of the Royal Astronomical Society, 433(1), 498-505.
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  Abstract: We report the detection of CO(1-0) line emission in the bright, lensed star-forming galaxies SPT-S 233227-5358.5 (z = 2.73) and SPT-S 053816-5030.8 (z = 2.78), using the Australia Telescope Compact Array. Both galaxies were discovered in a large-area millimetre survey with the South Pole Telescope (SPT) and found to be gravitationally lensed by intervening structures. The measured CO intensities imply galaxies with molecular gas masses of (3.2 ± 0.5) × 1010(μ/15)-1(XCO/0.8) and (1.7 ± 0.3) × 1010(μ/20)-1(XCO/0.8)M·, and gas depletion time-scales of 4.9 × 107(XCO/0.8) and 2.6 × 107(XCO/0.8) yr, respectively, where μ corresponds to the lens magnification and XCO is the CO luminosity to gas mass conversion factor. In the case of SPT-S 053816-5030.8, we also obtained significant detections of the rest-frame 115.7 and 132.4 GHz radio continuum. Based on the radio-to-infrared spectral energy distribution and an assumed synchrotron spectral index, we find that 42 ± 10 and 55 ±13 per cent of the flux at rest-frame 115.7 and 132.4 GHz arises from free-free emission. We find a radio-derived intrinsic star formation rate of 470 ± 170M· yr-1, consistent within the uncertainties with the infrared estimate. Based on the morphology of this object in the source plane, the derived gas mass and the possible flattening of the radio spectral index towards low frequencies, we argue that SPT-S 053816-5030.8 exhibits properties compatible with a scaled-up local ultraluminous infrared galaxy. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
• Benson, B. A., Haan, T. D., Dudley, J. P., Reichardt, C. L., Aird, K. A., Andersson, K., Armstrong, R., Ashby, M. L., Bautz, M., Bayliss, M., Bazin, G., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., , Desai, S., et al. (2013). Cosmological constraints from sunyaev-zel'dovich-selected clusters with X-ray observations in the first 178 deg² of the south pole telescope survey. Astrophysical Journal, 763(2).
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  Abstract: We use measurements from the South Pole Telescope (SPT) Sunyaev-Zel'dovich (SZ) cluster survey in combination with X-ray measurements to constrain cosmological parameters. We present a statistical method that fits for the scaling relations of the SZ and X-ray cluster observables with mass while jointly fitting for cosmology. The method is generalizable to multiple cluster observables, and self-consistently accounts for the effects of the cluster selection and uncertainties in cluster mass calibration on the derived cosmological constraints. We apply this method to a data set consisting of an SZ-selected catalog of 18 galaxy clusters at z > 0.3 from the first 178 deg2 of the 2500 deg2 SPT-SZ survey, with 14 clusters having X-ray observations from either Chandra or XMM-Newton. Assuming a spatially flat ΛCDM cosmological model, we find the SPT cluster sample constrains σ8(Ωm/0.25)0.30 = 0.785 ± 0.037. In combination with measurements of the cosmic microwave background (CMB) power spectrum from the SPT and the seven-year Wilkinson Microwave Anisotropy Probe data, the SPT cluster sample constrains σ8 = 0.795 ± 0.016 and Ωm= 0.255 ± 0.016, a factor of 1.5 improvement on each parameter over the CMB data alone. We consider several extensions beyond the ΛCDM model by including the following as free parameters: the dark energy equation of state (w), the sum of the neutrino masses (Σm ν), the effective number of relativistic species (N eff), and a primordial non-Gaussianity (f NL). We find that adding the SPT cluster data significantly improves the constraints on w and Σm ν beyond those found when using measurements of the CMB, supernovae, baryon acoustic oscillations, and the Hubble constant. Considering each extension independently, we best constrain w = -0.973 ± 0.063 and the sum of neutrino masses Σm ν < 0.28 eV at 95% confidence, a factor of 1.25 and 1.4 improvement, respectively, over the constraints without clusters. Assuming a ΛCDM model with a free N eff and Σm ν, we measure N eff = 3.91 ± 0.42 and constrain Σm ν < 0.63 eV at 95% confidence. We also use the SPT cluster sample to constrain f NL = -220 ± 317, consistent with zero primordial non-Gaussianity. Finally, we discuss the current systematic limitations due to the cluster mass calibration, and future improvements for the recently completed 2500 deg2 SPT-SZ survey. The survey has detected ∼500 clusters with a median redshift of ∼0.5 and a median mass of ∼2.3 × 10 14 M h-1 and, when combined with an improved cluster mass calibration and existing external cosmological data sets will significantly improve constraints on w. © 2013. The American Astronomical Society. All rights reserved..
• Bothwell, M. S., Aguirre, J. E., Chapman, S. C., Marrone, D. P., Vieira, J. D., Ashby, M. L., Aravena, M., Benson, B. A., Bock, J. J., Bradford, C. M., Brodwin, M., Carlstrom, J. E., Crawford, T. M., Breuck, C. D., Downes, T. P., Fassnacht, C. D., Gonzalez, A. H., Greve, T. R., Gullberg, B., , Hezaveh, Y., et al. (2013). SPT 0538-50: Physical conditions in the interstellar medium of a strongly lensed dusty star-forming galaxy at z = 2.8. Astrophysical Journal, 779(1).
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  Abstract: We present observations of SPT-S J053816-5030.8, a gravitationally lensed dusty star-forming galaxy (DSFG) at z = 2.7817 that was first discovered at millimeter wavelengths by the South Pole Telescope. SPT 0538-50 is typical of the brightest sources found by wide-field millimeter-wavelength surveys, being lensed by an intervening galaxy at moderate redshift (in this instance, at z = 0.441). We present a wide array of multi-wavelength spectroscopic and photometric data on SPT 0538-50, including data from ALMA, Herschel PACS and SPIRE, Hubble, Spitzer, the Very Large Telescope, ATCA, APEX, and the Submillimeter Array. We use high-resolution imaging from the Hubble Space Telescope to de-blend SPT 0538-50, separating DSFG emission from that of the foreground lens. Combined with a source model derived from ALMA imaging (which suggests a magnification factor of 21 ± 4), we derive the intrinsic properties of SPT 0538-50, including the stellar mass, far-IR luminosity, star formation rate, molecular gas mass, and - using molecular line fluxes - the excitation conditions within the interstellar medium. The derived physical properties argue that we are witnessing compact, merger-driven star formation in SPT 0538-50 similar to local starburst galaxies and unlike that seen in some other DSFGs at this epoch. © 2013. The American Astronomical Society. All rights reserved..
• Geach, J. E., Hickox, R. C., Bleem, L. E., Brodwin, M., Holder, G. P., Aird, K. A., Benson, B. A., Bhattacharya, S., Carlstrom, J. E., Chang, C. L., Cho, H. -., Crawford, T. M., Crites, A. T., Haan, T. D., Dobbs, M. A., Dudley, J., George, E. M., Hainline, K. N., Halverson, N. W., , Holzapfel, W. L., et al. (2013). A direct measurement of the linear bias of mid-infrared-selected quasars at z ≈ 1 using cosmic microwave background lensing. Astrophysical Journal Letters, 776(2).
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  Abstract: We measure the cross-power spectrum of the projected mass density as traced by the convergence of the cosmic microwave background lensing field from the South Pole Telescope (SPT) and a sample of Type 1 and 2 (unobscured and obscured) quasars at 〈z〉 ∼ 1 selected with the Wide-field Infrared Survey Explorer, over 2500 deg2. The cross-power spectrum is detected at ≈7σ, and we measure a linear bias b = 1.61 ± 0.22, consistent with clustering analyses. Using an independent lensing map, derived from Planck observations, to measure the cross-spectrum, we find excellent agreement with the SPT analysis. The bias of the combined sample of Type 1 and 2 quasars determined in this work is similar to that previously determined for Type 1 quasars alone; we conclude that obscured and unobscured quasars trace the matter field in a similar way. This result has implications for our understanding of quasar unification and evolution schemes. © 2013. The American Astronomical Society. All rights reserved.
• Hezaveh, Y. D., Marrone, D. P., Fassnacht, C. D., Spilker, J. S., Vieira, J. D., Aguirre, J. E., Aird, K. A., Aravena, M., Ashby, M. L., Bayliss, M., Benson, B. A., Bleem, L. E., Bothwell, M., Brodwin, M., Carlstrom, J. E., Chang, C. L., Chapman, S. C., Crawford, T. M., Crites, A. T., , Breuck, C. D., et al. (2013). Alma observations of spt-discovered, strongly lensed, dusty, star-forming galaxies. Astrophysical Journal, 767(2).
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  Abstract: We present Atacama Large Millimeter/submillimeter Array (ALMA) 860 μm imaging of four high-redshift (z = 2.8-5.7) dusty sources that were detected using the South Pole Telescope (SPT) at 1.4 mm and are not seen in existing radio to far-infrared catalogs. At 1.″5 resolution, the ALMA data reveal multiple images of each submillimeter source, separated by 1″-3″, consistent with strong lensing by intervening galaxies visible in near-IR imaging of these sources. We describe a gravitational lens modeling procedure that operates on the measured visibilities and incorporates self-calibration- like antenna phase corrections as part of the model optimization, which we use to interpret the source structure. Lens models indicate that SPT0346-52, located at z = 5.7, is one of the most luminous and intensely star-forming sources in the universe with a lensing corrected FIR luminosity of 3.7 × 10 13 L and star formation surface density of 4200 M⊙yr -1 kpc-2. We find magnification factors of 5 to 22, with lens Einstein radii of 1.″1-2.″0 and Einstein enclosed masses of 1.6-7.2 × 1011 M⊙. These observations confirm the lensing origin of these objects, allow us to measure their intrinsic sizes and luminosities, and demonstrate the important role that ALMA will play in the interpretation of lensed submillimeter sources. © 2013. The American Astronomical Society. All rights reserved.
• Hezaveh, Y., Dalal, N., Holder, G., Kuhlen, M., Marrone, D., Murray, N., & Vieira, J. (2013). Dark matter substructure detection using spatially resolved spectroscopy of lensed dusty galaxies. Astrophysical Journal, 767(1).
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  Abstract: We investigate how strong lensing of dusty, star-forming galaxies (DSFGs) by foreground galaxies can be used as a probe of dark matter halo substructure. We find that spatially resolved spectroscopy of lensed sources allows dramatic improvements to measurements of lens parameters. In particular, we find that modeling of the full, three-dimensional (angular position and radial velocity) data can significantly facilitate substructure detection, increasing the sensitivity of observables to lower mass subhalos. We carry out simulations of lensed dusty sources observed by early ALMA (Cycle 1) and use a Fisher matrix analysis to study the parameter degeneracies and mass detection limits of this method. We find that even with conservative assumptions, it is possible to detect galactic dark matter subhalos of ∼108 M® with high significance in most lensed DSFGs. Specifically, we find that in typical DSFG lenses, there is a ∼55% probability of detecting a substructure with M > 108 M® with more than 5σ detection significance in each lens, if the abundance of substructure is consistent with previous lensing results. The full ALMA array, with its significantly enhanced sensitivity and resolution, should improve these estimates considerably. Given the sample of ∼100 lenses provided by surveys such as the South Pole Telescope, our understanding of dark matter substructure in typical galaxy halos is poised to improve dramatically over the next few years. © 2013. The American Astronomical Society. All rights reserved..
• Holder, G. P., Viero, M. P., Zahn, O., Aird, K. A., Benson, B. A., Bhattacharya, S., Bleem, L. E., Bock, J., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. -., Conley, A., Crawford, T. M., Crites, A. T., Haan, T. D., Dobbs, M. A., Dudley, J., George, E. M., , Halverson, N. W., et al. (2013). A cosmic microwave background lensing mass map and its correlation with the cosmic infrared background. Astrophysical Journal Letters, 771(1).
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  Abstract: We use a temperature map of the cosmic microwave background (CMB) obtained using the South Pole Telescope at 150 GHz to construct a map of the gravitational convergence to z ∼ 1100, revealing the fluctuations in the projected mass density. This map shows individual features that are significant at the ∼4σ level, providing the first image of CMB lensing convergence. We cross-correlate this map with Herschel/SPIRE maps covering 90 deg2 at wavelengths of 500, 350, and 250 μm. We show that these submillimeter (submm) wavelength maps are strongly correlated with the lensing convergence map, with detection significances in each of the three submm bands ranging from 6.7σ to 8.8σ. We fit the measurement of the cross power spectrum assuming a simple constant bias model and infer bias factors of b = 1.3-1.8, with a statistical uncertainty of 15%, depending on the assumed model for the redshift distribution of the dusty galaxies that are contributing to the Herschel/SPIRE maps. © 2013. The American Astronomical Society. All rights reserved.
• Lu, R., Fish, V. L., Akiyama, K., Doeleman, S. S., Algaba, J. C., Bower, G. C., Brinkerink, C., Chamberlin, R., Crew, G., Cappallo, R. J., Dexter, M., Freund, R., Friberg, P., Gurwell, M. A., T., P., Honma, M., Inoue, M., Jorstad, S. G., Krichbaum, T. P., , Loinard, L., et al. (2013). Fine-scale structure of the quasar 3C 279 measured with 1.3 mm very long baseline interferometry. Astrophysical Journal, 772(1).
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  Abstract: We report results from five day very long baseline interferometry observations of the well-known quasar 3C 279 at 1.3 mm (230 GHz) in 2011. The measured nonzero closure phases on triangles including stations in Arizona, California, and Hawaii indicate that the source structure is spatially resolved. We find an unusual inner jet direction at scales of ∼1 pc extending along the northwest-southeast direction (P.A. = 127° ± 3°), as opposed to other (previously) reported measurements on scales of a few parsecs showing inner jet direction extending to the southwest. The 1.3 mm structure corresponds closely with that observed in the central region of quasi-simultaneous super-resolution Very Long Baseline Array images at 7 mm. The closure phase changed significantly on the last day when compared with the rest of observations, indicating that the inner jet structure may be variable on daily timescales. The observed new direction of the inner jet shows inconsistency with the prediction of a class of jet precession models. Our observations indicate a brightness temperature of ∼8 × 1010 K in the 1.3 mm core, much lower than that at centimeter wavelengths. Observations with better uv coverage and sensitivity in the coming years will allow the discrimination between different structure models and will provide direct images of the inner regions of the jet with 20-30 μas (5-7 light months) resolution. © 2013. The American Astronomical Society. All rights reserved.
• McDonald, M., Benson, B. A., Vikhlinin, A., Stalder, B., Bleem, L. E., Haan, T. D., Lin, H. W., Aird, K. A., Ashby, M. L., Bautz, M. W., Bayliss, M., Bocquet, S., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., , Desai, S., et al. (2013). The growth of cool cores and evolution of cooling properties in a sample of 83 galaxy clusters at 0.3 < z < 1.2 selected from the SPT-SZ survey. Astrophysical Journal, 774(1).
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  Abstract: We present first results on the cooling properties derived from Chandra X-ray observations of 83 high-redshift (0.3 < z < 1.2) massive galaxy clusters selected by their Sunyaev-Zel'dovich signature in the South Pole Telescope data. We measure each cluster's central cooling time, central entropy, and mass deposition rate, and compare these properties to those for local cluster samples. We find no significant evolution from z 0 to z 1 in the distribution of these properties, suggesting that cooling in cluster cores is stable over long periods of time. We also find that the average cool core entropy profile in the inner 100 kpc has not changed dramatically since z 1, implying that feedback must be providing nearly constant energy injection to maintain the observed "entropy floor" at 10 keV cm2. While the cooling properties appear roughly constant over long periods of time, we observe strong evolution in the gas density profile, with the normalized central density (ρg, 0/ρcrit) increasing by an order of magnitude from z 1 to z 0. When using metrics defined by the inner surface brightness profile of clusters, we find an apparent lack of classical, cuspy, cool-core clusters at z > 0.75, consistent with earlier reports for clusters at z > 0.5 using similar definitions. Our measurements indicate that cool cores have been steadily growing over the 8 Gyr spanned by our sample, consistent with a constant, 150 M yr-1 cooling flow that is unable to cool below entropies of 10 keV cm2 and, instead, accumulates in the cluster center. We estimate that cool cores began to assemble in these massive systems at , which represents the first constraints on the onset of cooling in galaxy cluster cores. At high redshift (z ≳ 0.75), galaxy clusters may be classified as "cooling flows" (low central entropy, cooling time) but not "cool cores" (cuspy surface brightness profile), meaning that care must be taken when classifying these high-z systems. We investigate several potential biases that could conspire to mimic this cool core evolution and are unable to find a bias that has a similar redshift dependence and a substantial amplitude. © 2013. The American Astronomical Society. All rights reserved..
• Mocanu, L. M., Crawford, T. M., Vieira, J. D., Aird, K. A., Aravena, M., Austermann, J. E., Benson, B. A., Béthermin, M., Bleem, L. E., Bothwell, M., Carlstrom, J. E., Chang, C. L., Chapman, S., Cho, H. -., Crites, A. T., Haan, T. D., Dobbs, M. A., Everett, W. B., George, E. M., , Halverson, N. W., et al. (2013). Extragalactic millimeter-wave point-source catalog, number counts and statistics from 771 deg² of the SPT-SZ survey. Astrophysical Journal, 779(1).
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  Abstract: We present a point-source catalog from 771 deg2 of the South Pole Telescope Sunyaev-Zel'dovich survey at 95, 150, and 220 GHz. We detect 1545 sources above 4.5σ significance in at least one band. Based on their relative brightness between survey bands, we classify the sources into two populations, one dominated by synchrotron emission from active galactic nuclei, and one dominated by thermal emission from dust-enshrouded star-forming galaxies. We find 1238 synchrotron and 307 dusty sources. We cross-match all sources against external catalogs and find 189 unidentified synchrotron sources and 189 unidentified dusty sources. The dusty sources without counterparts are good candidates for high-redshift, strongly lensed submillimeter galaxies. We derive number counts for each population from 1 Jy down to roughly 11, 4, and 11 mJy at 95, 150, and 220 GHz. We compare these counts with galaxy population models and find that none of the models we consider for either population provide a good fit to the measured counts in all three bands. The disparities imply that these measurements will be an important input to the next generation of millimeter-wave extragalactic source population models. © 2013. The American Astronomical Society. All rights reserved..
• Plagge, T. J., Marrone, D. P., Abdulla, Z., Bonamente, M., Carlstrom, J. E., Gralla, M., Greer, C. H., Joy, M., Lamb, J. W., Leitch, E. M., Mantz, A., Muchovej, S., & Woody, D. (2013). Carma measurements of the Sunyaev-Zel'dovich effect in RX J1347.5-1145. Astrophysical Journal, 770(2).
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  Abstract: We demonstrate the Sunyaev-Zel'dovich (SZ) effect imaging capabilities of the Combined Array for Research in Millimeter-wave Astronomy (CARMA) by presenting an SZ map of the galaxy cluster RX J1347.5-1145. By combining data from multiple CARMA bands and configurations, we are able to capture the structure of this cluster over a wide range of angular scales, from its bulk properties to its core morphology. We find that roughly 9% of this cluster's thermal energy is associated with sub-arcminute-scale structure imparted by a merger, illustrating the value of high-resolution SZ measurements for pursuing cluster astrophysics and for understanding the scatter in SZ scaling relations. We also find that the cluster's SZ signal is lower in amplitude than suggested by a spherically symmetric model derived from X-ray data, consistent with compression along the line of sight relative to the plane of the sky. Finally, we discuss the impact of upgrades currently in progress that will further enhance CARMA's power as an SZ imaging instrument. © 2013. The American Astronomical Society. All rights reserved..
• Reichardt, C. L., Stalder, B., Bleem, L. E., Montroy, T. E., Aird, K. A., Andersson, K., Armstrong, R., Ashby, M. L., Bautz, M., Bayliss, M., Bazin, G., Benson, B. A., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., , Haan, T. D., et al. (2013). Galaxy clusters discovered via the sunyaev-zel'dovich effect in the first 720 square degrees of the south pole telescope survey. Astrophysical Journal, 763(2).
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  Abstract: We present a catalog of galaxy cluster candidates, selected through their Sunyaev-Zel'dovich (SZ) effect signature in the first 720 deg2 of the South Pole Telescope (SPT) survey. This area was mapped with the SPT in the 2008 and 2009 austral winters to a depth of ∼18 μKCMB-arcmin at 150 GHz; 550 deg2 of it was also mapped to ∼44 μK CMB-arcmin at 95 GHz. Based on optical imaging of all 224 candidates and near-infrared imaging of the majority of candidates, we have found optical and/or infrared counterparts for 158, which we then classify as confirmed galaxy clusters. Of these 158 clusters, 135 were first identified as clusters in SPT data, including 117 new discoveries reported in this work. This catalog triples the number of confirmed galaxy clusters discovered through the SZ effect. We report photometrically derived (and in some cases spectroscopic) redshifts for confirmed clusters and redshift lower limits for the remaining candidates. The catalog extends to high redshift with a median redshift of z = 0.55 and maximum confirmed redshift of z = 1.37. Forty-five of the clusters have counterparts in the ROSAT bright or faint source catalogs from which we estimate X-ray fluxes. Based on simulations, we expect the catalog to be nearly 100% complete above M 500 ≈ 5 × 1014 M h-170 at z ≳ 0.6. There are 121 candidates detected at signal-to-noise ratio greater than five, at which the catalog purity is measured to be 95%. From this high-purity subsample, we exclude the z < 0.3 clusters and use the remaining 100 candidates to improve cosmological constraints following the method presented by Benson et al. Adding the cluster data to CMB + BAO + H 0 data leads to a preference for non-zero neutrino masses while only slightly reducing the upper limit on the sum of neutrino masses to ∑m ν < 0.38 eV (95% CL). For a spatially flat wCDM cosmological model, the addition of this catalog to the CMB + BAO + H 0 + SNe results yields σ8 = 0.807 ± 0.027 and w = -1.010 ± 0.058, improving the constraints on these parameters by a factor of 1.4 and 1.3, respectively. The larger cluster catalog presented in this work leads to slight improvements in cosmological constraints from those presented by Benson et al. These cosmological constraints are currently limited by uncertainty in the cluster mass calibration, not the size or quality of the cluster catalog. A multi-wavelength observation program to improve the cluster mass calibration will make it possible to realize the full potential of the final 2500 deg2 SPT cluster catalog to constrain cosmology. © 2013. The American Astronomical Society. All rights reserved..
• Stalder, B., Ruel, J., Šuhada, R., Brodwin, M., Aird, K. A., Andersson, K., Armstrong, R., Ashby, M. L., Bautz, M., Bayliss, M., Bazin, G., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., , Haan, T. D., et al. (2013). SPT-CL J0205-5829: A z = 1.32 Evolved massive galaxy cluster in the south pole telescope sunyaev-zel'dovich effect survey. Astrophysical Journal, 763(2).
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  Abstract: The galaxy cluster SPT-CL J0205-5829 currently has the highest spectroscopically confirmed redshift, z = 1.322, in the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey. XMM-Newton observations measure a core-excluded temperature of TX = 8.7+1.0-0.8 keV producing a mass estimate that is consistent with the Sunyaev-Zel'dovich- derived mass. The combined SZ and X-ray mass estimate of M 500 = (4.8 ± 0.8) × 1014 h -170 M makes it the most massive known SZ-selected galaxy cluster at z > 1.2 and the second most massive at z > 1. Using optical and infrared observations, we find that the brightest galaxies in SPT-CL J0205-5829 are already well evolved by the time the universe was
• Vieira, J. D., Marrone, D. P., Chapman, S. C., Breuck, C. D., Hezaveh, Y. D., Wei, A., Aguirre, J. E., Aird, K. A., Aravena, M., Ashby, M. L., Bayliss, M., Benson, B. A., Biggs, A. D., Bleem, L. E., Bock, J. J., Bothwell, M., Bradford, C. M., Brodwin, M., Carlstrom, J. E., , Chang, C. L., et al. (2013). Dusty starburst galaxies in the early Universe as revealed by gravitational lensing. Nature, 495(7441), 344-347.
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  PMID: 23485967;Abstract: In the past decade, our understanding of galaxy evolution has been revolutionized by the discovery that luminous, dusty starburst galaxies were 1,000 times more abundant in the early Universe than at present. It has, however, been difficult to measure the complete redshift distribution of these objects, especially at the highest redshifts (z>4). Here we report a redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources. High-resolution imaging demonstrates that these sources are strongly gravitationally lensed by foreground galaxies. We detect spectral lines in 23 out of 26 sources and multiple lines in 12 of those 23 sources, from which we obtain robust, unambiguous redshifts. At least 10 of the sources are found to lie at z>4, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought. Models of lens geometries in the sample indicate that the background objects are ultra-luminous infrared galaxies, powered by extreme bursts of star formation. © 2013 Macmillan Publishers Limited. All rights reserved.
• Wei, A., Breuck, C. D., Marrone, D. P., Vieira, J. D., Aguirre, J. E., Aird, K. A., Aravena, M., Ashby, M. L., Bayliss, M., Benson, B. A., Béthermin, M., Biggs, A. D., Bleem, L. E., Bock, J. J., Bothwell, M., Bradford, C. M., Brodwin, M., Carlstrom, J. E., Chang, C. L., , Chapman, S. C., et al. (2013). Alma redshifts of millimeter-selected galaxies from the SPT survey: The redshift distribution of dusty star-forming galaxies. Astrophysical Journal, 767(1).
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  Abstract: Using the Atacama Large Millimeter/submillimeter Array, we have conducted a blind redshift survey in the 3 mm atmospheric transmission window for 26 strongly lensed dusty star-forming galaxies (DSFGs) selected with the South Pole Telescope. The sources were selected to have S1.4 mm > 20 mJy and a dust-like spectrum and, to remove low-z sources, not have bright radio (S843 MHz < 6 mJy) or far-infrared counterparts (S 100 μm < 1 Jy, S60 μm < 200 mJy). We robustly detect 44 line features in our survey, which we identify as redshifted emission lines of 12CO, 13CO, C I, H2O, and H2O +. We find one or more spectral features in 23 sources yielding a ∼90% detection rate for this survey; in 12 of these sources we detect multiple lines, while in 11 sources we detect only a single line. For the sources with only one detected line, we break the redshift degeneracy with additional spectroscopic observations if available, or infer the most likely line identification based on photometric data. This yields secure redshifts for ∼70% of the sample. The three sources with no lines detected are tentatively placed in the redshift desert between 1.7 < z < 2.0. The resulting mean redshift of our sample is = 3.5. This finding is in contrast to the redshift distribution of radio-identified DSFGs, which have a significantly lower mean redshift of = 2.3 and for which only 10%-15% of the population is expected to be at z > 3. We discuss the effect of gravitational lensing on the redshift distribution and compare our measured redshift distribution to that of models in the literature. © 2013. The American Astronomical Society. All rights reserved.
• Yefremenko, V., Ade, P., Aird, K., Austermann, J., Beall, J., Becker, D., Benson, B., Bleem, L., Britton, J., Chang, C. L., Carlstrom, J., Cho, H., Haan, T. D., Crawford, T., Crites, A., Datesman, A., Dobbs, M., Everett, W., Ewall-Wice, A., , George, E., et al. (2013). Design and fabrication of 90 GHz TES polarimeter detectors for the south pole telescope. IEEE Transactions on Applied Superconductivity, 23(3).
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  Abstract: We present information about the design and fabrication of 90 GHz Transition Edge Sensor (TES) detectors deployed in the SPTpol camera for investigation of the cosmic microwave background (CMB) polarization signal. The 90 GHz portion of the camera consists of 180 individual feedhorn modules with dual polarization-sensitive detectors. We discuss microfabrication details and the characterization of detector elements. Each detector incorporates a dipole-like Pd-Au absorber and Mo/Au TES thermometer, suspended together on a rectangular silicon nitride (SiN) membrane via 6 long (640 \mu\hbox{m}) and narrow (10 \mu\hbox{m}) legs. The geometry of the SiN legs was optimized to provide the target thermal conductance of 200 pW/K in combination with mechanical robustness and reliability. The proximity effect in superconductor (Mo) and normal metal (Au) bilayers was utilized to obtain a TES operating temperature between 520 and 540 mK. Excellent superconducting properties (transition width < 1 mK) and T\rm c uniformity (< 3 mK) across 2 \prime\prime wafers were achieved by sputtering in a confocal system under a single vacuum using an independent RF bias applied to the substrate. Superconducting Nb dots patterned on the TES surface provided controllable broadening of the transition width. We report the results of transition measurements, along with characterization of film morphology. © 2002-2011 IEEE.
• Austermann, J. E., Aird, K. A., Beall, J. A., Becker, D., Bender, A., Benson, B. A., Bleem, L. E., Britton, J., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Cho, H. -., Crawford, T. M., Crites, A. T., Datesman, A., Haan, T. D., Dobbs, M. A., George, E. M., Halverson, N. W., , Harrington, N., et al. (2012). SPTpol: An instrument for CMB polarization measurements with the South Pole Telescope. Proceedings of SPIE - The International Society for Optical Engineering, 8452.
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  Abstract: SPTpol is a dual-frequency polarization-sensitive camera that was deployed on the 10-meter South Pole Telescope in January 2012. SPTpol will measure the polarization anisotropy of the cosmic microwave background (CMB) on angular scales spanning an arcminute to several degrees. The polarization sensitivity of SPTpol will enable a detection of the CMB "B-mode" polarization from the detection of the gravitational lensing of the CMB by large scale structure, and a detection or improved upper limit on a primordial signal due to inflationary gravity waves. The two measurements can be used to constrain the sum of the neutrino masses and the energy scale of inflation. These science goals can be achieved through the polarization sensitivity of the SPTpol camera and careful control of systematics. The SPTpol camera consists of 768 pixels, each containing two transition-edge sensor (TES) bolometers coupled to orthogonal polarizations, and a total of 1536 bolometers. The pixels are sensitive to light in one of two frequency bands centered at 90 and 150 GHz, with 180 pixels at 90 GHz and 588 pixels at 150 GHz. The SPTpol design has several features designed to control polarization systematics, including: single-moded feedhorns with low cross-polarization, bolometer pairs well-matched to difference atmospheric signals, an improved ground shield design based on far-sidelobe measurements of the SPT, and a small beam to reduce temperature to polarization leakage. We present an overview of the SPTpol instrument design, project status, and science projections. © 2012 SPIE.
• Barry, P. S., Shirokoff, E., Kovács, A., Reck, T. J., Hailey-Dunsheath, S., McKenney, C. M., Swenson, L. J., Hollister, M. I., Leduc, H. G., Doyle, S., O'Brient, R., Llombart, N., Marrone, D., Chattopadhyay, G., Day, P. K., Padin, S., Bradford, C. M., Mauskopf, P. D., & Zmuidzinas, J. (2012). Electromagnetic design for SuperSpec; a lithographically-patterned millimetre-wave spectrograph. Proceedings of SPIE - The International Society for Optical Engineering, 8452.
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  Abstract: SuperSpec is an innovative, fully planar, compact spectrograph for mm/sub-mm astronomy. SuperSpec is based on a superconducting filter-bank consisting of a series of planar half-wavelength filters to divide up the incoming, broadband radiation. The power in each filter is then coupled into titanium nitride lumped element kinetic inductance detectors, facilitating the read out of a large number of filter elements. We will present electromagnetic simulations of the different components that will make up an R = 700 prototype instrument. Based on these simulations, we discuss optimisation of the coupling between the antenna, transmission line, filters and detectors. © 2012 SPIE.
• Bleem, L. E., Engelen, A. V., Holder, G. P., Aird, K. A., Armstrong, R., Ashby, M. L., Becker, M. R., Benson, B. A., Biesiadzinski, T., Brodwin, M., Busha, M. T., Carlstrom, J. E., Chang, C. L., Cho, H. M., Crawford, T. M., Crites, A. T., Haan, T. D., Desai, S., Dobbs, M. A., , Doré, O., et al. (2012). A measurement of the correlation of galaxy surveys with CMB lensing convergence maps from the south pole telescope. Astrophysical Journal Letters, 753(1).
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  Abstract: We compare cosmic microwave background lensing convergence maps derived from South Pole Telescope (SPT) data with galaxy survey data from the Blanco Cosmology Survey, WISE, and a new large Spitzer/IRAC field designed to overlap with the SPT survey. Using optical and infrared catalogs covering between 17 and 68deg2 of sky, we detect a correlation between the SPT convergence maps and each of the galaxy density maps at >4σ, with zero correlation robustly ruled out in all cases. The amplitude and shape of the cross-power spectra are in good agreement with theoretical expectations and the measured galaxy bias is consistent with previous work. The detections reported here utilize a small fraction of the full 2500deg2 SPT survey data and serve as both a proof of principle of the technique and an illustration of the potential of this emerging cosmological probe. © 2012. The American Astronomical Society. All rights reserved..
• Bonamente, M., Hasler, N., Bulbul, E., Carlstrom, J. E., Culverhouse, T. L., Gralla, M., Greer, C., Hawkins, D., Hennessy, R., Joy, M., Kolodziejczak, J., Lamb, J. W., Landry, D., Leitch, E. M., Marrone, D. P., Miller, A., Mroczkowski, T., Muchovej, S., Plagge, T., , Pryke, C., et al. (2012). Comparison of pressure profiles of massive relaxed galaxy clusters using the Sunyaev-Zel'dovich and x-ray data. New Journal of Physics, 14.
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  Abstract: We present the Sunyaev-Zel'dovich (SZ) effect observations of a sample of 25 massive relaxed galaxy clusters observed with the Sunyaev-Zel'dovich array (SZA), an eight-element interferometer that is part of the Combined Array for Research in Millimeter-wave Astronomy (CARMA). We performed an analysis of new SZA data and archival Chandra observations of this sample to investigate the integrated pressure-a proxy for cluster mass-determined from x-ray and SZ observations, two independent probes of the intra-cluster medium (ICM). This analysis makes use of a model for the ICM introduced by Bulbul (2010 Astrophys. J. 720 1038) which can be applied simultaneously to the SZ and x-ray data. With this model, we estimated the pressure profile for each cluster using a joint analysis of the SZ and x-ray data, and using the SZ data alone. We found that the integrated pressures measured from the x-ray and SZ data are consistent. This conclusion is in agreement with recent results obtained using WMAP and Planck data, confirming that SZ and x-ray observations of massive clusters detect the same amount of thermal pressure from the ICM. To test for possible biases introduced by our choice of model, we also fitted the SZ data using the universal pressure profile proposed by Arnaud (2010 Astron. Astrophys. 517 A92) and found consistency between the two models out to r500 in the pressure profiles and integrated pressures. © IOP Publishing Ltd and Deutsche Physikalische Gesellschaft.
• George, E. M., Ade, P., Aird, K. A., Austermann, J. E., Beall, J. A., Becker, D., Bender, A., Benson, B. A., Bleem, L. E., Britton, J., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Cho, H. -., Crawford, T. M., Crites, A. T., Datesman, A., Haan, T. D., Dobbs, M. A., , Everett, W., et al. (2012). Performance and on-sky optical characterization of the SPTpol instrument. Proceedings of SPIE - The International Society for Optical Engineering, 8452.
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  Abstract: In January 2012, the 10m South Pole Telescope (SPT) was equipped with a polarization-sensitive camera, SPTpol, in order to measure the polarization anisotropy of the cosmic microwave background (CMB). Measurements of the polarization of the CMB at small angular scales (∼several arcminutes) can detect the gravitational lensing of the CMB by large scale structure and constrain the sum of the neutrino masses. At large angular scales (∼few degrees) CMB measurements can constrain the energy scale of Ination. SPTpol is a two-color mm-wave camera that consists of 180 polarimeters at 90 GHz and 588 polarimeters at 150 GHz, with each polarimeter consisting of a dual transition edge sensor (TES) bolometers. The full complement of 150 GHz detectors consists of 7 arrays of 84 ortho-mode transducers (OMTs) that are stripline coupled to two TES detectors per OMT, developed by the TRUCE collaboration and fabricated at NIST. Each 90 GHz pixel consists of two antenna-coupled absorbers coupled to two TES detectors, developed with Argonne National Labs. The 1536 total detectors are read out with digital frequency-domain multiplexing (DfMUX). The SPTpol deployment represents the first on-sky tests of both of these detector technologies, and is one of the first deployed instruments using DfMUX readout technology. We present the details of the design, commissioning, deployment, on-sky optical characterization and detector performance of the complete SPTpol focal plane. © 2012 SPIE.
• Greve, T. R., Vieira, J. D., Wei, A., Aguirre, J. E., Aird, K. A., Ashby, M. L., Benson, B. A., Bleem, L. E., Bradford, C. M., Brodwin, M., Carlstrom, J. E., Chang, C. L., Chapman, S. C., Crawford, T. M., Breuck, C. D., Haan, T. D., Dobbs, M. A., Downes, T., Fassnacht, C. D., , Fazio, G., et al. (2012). Submillimeter observations of millimeter bright galaxies discovered by the south pole telescope. Astrophysical Journal, 756(1).
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  Abstract: We present APEX SABOCA 350 μm and LABOCA 870 μm observations of 11 representative examples of the rare, extremely bright (S 1.4 mm > 15 mJy), dust-dominated millimeter-selected galaxies recently discovered by the South Pole Telescope. All 11 sources are robustly detected with LABOCA with 40 mJy < S 870 μm < 130 mJy, approximately an order of magnitude higher than the canonical submillimeter galaxy (SMG) population. Six of the sources are also detected by SABOCA at >3σ, with the detections or upper limits providing a key constraint on the shape of the spectral energy distribution (SED) near its peak. We model the SEDs of these galaxies using a simple modified blackbody and perform the same analysis on samples of SMGs of known redshift from the literature. These calibration samples inform the distribution of dust temperature for similar SMG populations, and this dust temperature prior allows us to derive photometric redshift estimates and far-infrared luminosities for the sources. We find a median redshift of , higher than the inferred for the normal SMG population. We also derive the apparent size of the sources from the temperature and apparent luminosity, finding them to appear larger than our unlensed calibration sample, which supports the idea that these sources are gravitationally magnified by massive structures along the line of sight. © © 2012. The American Astronomical Society. All rights reserved..
• Hasler, N., Bulbul, E., Bonamente, M., Carlstrom, J. E., Culverhouse, T. L., Gralla, M., Greer, C., Hawkins, D., Hennessy, R., Joy, M., Kolodziejczak, J., Lamb, J. W., Landry, D., Leitch, E. M., Mantz, A., Marrone, D. P., Miller, A., Mroczkowski, T., Muchovej, S., , Plagge, T., et al. (2012). Joint analysis of X-ray and Sunyaev-Zel'dovich observations of galaxy clusters using an analytic model of the intracluster medium. Astrophysical Journal, 748(2).
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  Abstract: We perform a joint analysis of X-ray and Sunyaev-Zel'dovich effect data using an analytic model that describes the gas properties of galaxy clusters. The joint analysis allows the measurement of the cluster gas mass fraction profile and Hubble constant independent of cosmological parameters. Weak cosmological priors are used to calculate the overdensity radius within which the gas mass fractions are reported. Such an analysis can provide direct constraints on the evolution of the cluster gas mass fraction with redshift. We validate the model and the joint analysis on high signal-to-noise data from the Chandra X-ray Observatory and the Sunyaev-Zel'dovich Array for two clusters, A2631 and A2204. © 2012. The American Astronomical Society. All rights reserved.
• Henning, J. W., Ade, P., Aird, K. A., Austermann, J. E., Beall, J. A., Becker, D., Benson, B. A., Bleem, L. E., Britton, J., Carlstrom, J. E., Chang, C. L., Cho, H. -., Crawford, T. M., Crites, A. T., Datesman, A., Haan, T. D., Dobbs, M. A., Everett, W., Ewall-Wice, A., , George, E. M., et al. (2012). Feedhorn-coupled TES polarimeter camera modules at 150 GHz for CMB polarization measurements with SPTpol. Proceedings of SPIE - The International Society for Optical Engineering, 8452.
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  Abstract: The SPTpol camera is a dichroic polarimetric receiver at 90 and 150 GHz. Deployed in January 2012 on the South Pole Telescope (SPT), SPTpol is looking for faint polarization signals in the Cosmic Microwave Background (CMB). The camera consists of 180 individual Transition Edge Sensor (TES) polarimeters at 90 GHz and seven 84-polarimeter camera modules (a total of 588 polarimeters) at 150 GHz. We present the design, dark characterization, and in-lab optical properties of the 150 GHz camera modules. The modules consist of photolithographed arrays of TES polarimeters coupled to silicon platelet arrays of corrugated feedhorns, both of which are fabricated at NIST-Boulder. In addition to mounting hardware and RF shielding, each module also contains a set of passive readout electronics for digital frequency-domain multiplexing. A single module, therefore, is fully functional as a miniature focal plane and can be tested independently. Across the modules tested before deployment, the detectors average a critical temperature of 478 mK, normal resistance R N of 1.2 Ω, unloaded saturation power of 22.5 pW, (detector-only) optical efficiency of ∼ 90%, and have electrothermal time constants < 1 ms in transition. © 2012 SPIE.
• Hezaveh, Y. D., Marrone, D. P., & Holder, G. P. (2012). Size bias and differential lensing of strongly lensed, dusty galaxies identified in wide-field surveys. Astrophysical Journal, 761(1).
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  Abstract: We address two selection effects that operate on samples of gravitationally lensed dusty galaxies identified in millimeter- and submillimeter-wavelength surveys. First, we point out the existence of a "size bias" in such samples: due to finite source effects, sources with higher observed fluxes are increasingly biased toward more compact objects. Second, we examine the effect of differential lensing in individual lens systems by modeling each source as a compact core embedded in an extended diffuse halo. Considering the ratio of magnifications in these two components, we find that at high overall magnifications, the compact component is amplified by a much larger factor than the diffuse component, but at intermediate magnifications (∼10) the probability of a larger magnification for the extended region is higher. Lens models determined from multi-frequency resolved imaging data are crucial to correct for this effect. © 2012. The American Astronomical Society. All rights reserved..
• High, F. W., Hoekstra, H., Leethochawalit, N., Haan, T. D., Abramson, L., Aird, K. A., Armstrong, R., Ashby, M. L., Bautz, M., Bayliss, M., Bazin, G., Benson, B. A., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Conroy, M., , Crawford, T. M., et al. (2012). Weak-lensing mass measurements of five galaxy clusters in the south pole telescope survey using Magellan/Megacam. Astrophysical Journal, 758(1).
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  Abstract: We use weak gravitational lensing to measure the masses of five galaxy clusters selected from the South Pole Telescope (SPT) survey, with the primary goal of comparing these with the SPT Sunyaev-Zel'dovich (SZ) and X-ray-based mass estimates. The clusters span redshifts 0.28 < z < 0.43 and have masses M 500 > 2 × 10 14 h -1 M ⊙, and three of the five clusters were discovered by the SPT survey. We observed the clusters in the g′r′i′ passbands with the Megacam imager on the Magellan Clay 6.5m telescope. We measure a mean ratio of weak-lensing (WL) aperture masses to inferred aperture masses from the SZ data, both within an aperture of R 500, SZ derived from the SZ mass, of 1.04 ± 0.18. We measure a mean ratio of spherical WL masses evaluated at R 500, SZ to spherical SZ masses of 1.07 ± 0.18, and a mean ratio of spherical WL masses evaluated at R 500, WL to spherical SZ masses of 1.10 ± 0.24. We explore potential sources of systematic error in the mass comparisons and conclude that all are subdominant to the statistical uncertainty, with dominant terms being cluster concentration uncertainty and N-body simulation calibration bias. Expanding the sample of SPT clusters with WL observations has the potential to significantly improve the SPT cluster mass calibration and the resulting cosmological constraints from the SPT cluster survey. These are the first WL detections using Megacam on the Magellan Clay telescope. © 2012. The American Astronomical Society. All rights reserved.
• Kovács, A., Barry, P. S., Bradford, C. M., Chattopadhyay, G., Day, P., Doyle, S., Hailey-Dunsheath, S., Hollister, M., McKenney, C., LeDuc, H. G., Llombart, N., Marrone, D. P., Mauskopf, P., O'Brient, R., Padin, S., Swenson, L. J., & Zmuidzinas, J. (2012). SuperSpec: Design concept and circuit simulations. Proceedings of SPIE - The International Society for Optical Engineering, 8452.
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  Abstract: SuperSpec is a pathfinder for future lithographic spectrometer cameras, which promise to energize extra-galactic astrophysics at (sub)millimeter wavelengths: delivering 200-500 kms-1 spectral velocity resolution over an octave bandwidth for every pixel in a telescope's field of view. We present circuit simulations that prove the concept, which enables complete millimeter-band spectrometer devices in just a few square-millimeter footprint. We evaluate both single-stage and two-stage channelizing filter designs, which separate channels into an array of broad-band detectors, such as bolometers or kinetic inductance detector (KID) devices. We discuss to what degree losses (by radiation or by absorption in the dielectric) and fabrication tolerances affect the resolution or performance of such devices, and what steps we can take to mitigate the degradation. Such design studies help us formulate critical requirements on the materials and fabrication process, and help understand what practical limits currently exist to the capabilities these devices can deliver today or over the next few years. © 2012 SPIE.
• Marrone, D. P., Smith, G. P., Okabe, N., Bonamente, M., Carlstrom, J. E., Culverhouse, T. L., Gralla, M., Greer, C. H., Hasler, N., Hawkins, D., Hennessy, R., Joy, M., Lamb, J. W., Leitch, E. M., Martino, R., Mazzotta, P., Miller, A., Mroczkowski, T., Muchovej, S., , Plagge, T., et al. (2012). LoCuSS: The Sunyaev-Zel'dovich effect and weak-lensing mass scaling relation. Astrophysical Journal, 754(2).
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  Abstract: We present the first weak-lensing-based scaling relation between galaxy cluster mass, M WL, and integrated Compton parameter Y sph. Observations of 18 galaxy clusters at z ≃ 0.2 were obtained with the Subaru 8.2m telescope and the Sunyaev-Zel'dovich Array. The M WL-Y sph scaling relations, measured at Δ = 500, 1000, and 2500 ρ c, are consistent in slope and normalization with previous results derived under the assumption of hydrostatic equilibrium (HSE). We find an intrinsic scatter in M WL at fixed Y sph of 20%, larger than both previous measurements of M HSE-Y sph scatter as well as the scatter in true mass at fixed Y sph found in simulations. Moreover, the scatter in our lensing-based scaling relations is morphology dependent, with 30%-40% larger M WL for undisturbed compared to disturbed clusters at the same Y sph at r 500. Further examination suggests that the segregation may be explained by the inability of our spherical lens models to faithfully describe the three-dimensional structure of the clusters, in particular, the structure along the line of sight. We find that the ellipticity of the brightest cluster galaxy, a proxy for halo orientation, correlates well with the offset in mass from the mean scaling relation, which supports this picture. This provides empirical evidence that line-of-sight projection effects are an important systematic uncertainty in lensing-based scaling relations. © 2012. The American Astronomical Society. All rights reserved..
• McDonald, M., Bayliss, M., Benson, B. A., Foley, R. J., Ruel, J., Sullivan, P., Veilleux, S., Aird, K. A., Ashby, M. L., Bautz, M., Bazin, G., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., , Haan, T. D., et al. (2012). A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies. Nature, 488(7411), 349-352.
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  PMID: 22895340;Abstract: In the cores of some clusters of galaxies the hot intracluster plasma is dense enough that it should cool radiatively in the clusters lifetime, leading to continuous cooling flows of gas sinking towards the cluster centre, yet no such cooling flow has been observed. The low observed star-formation rates and cool gas masses for these cool-core clusters suggest that much of the cooling must be offset by feedback to prevent the formation of a runaway cooling flow. Here we report X-ray, optical and infrared observations of the galaxy cluster SPT-CLJ2344-4243 (ref. 11) at redshift z = 0.596. These observations reveal an exceptionally luminous (8.2Ã-10 45 ergs-1) galaxy cluster that hosts an extremely strong cooling flow (around 3,820 solar masses a year). Further, the central galaxy in this cluster appears to be experiencing a massive starburst (formation of around 740 solar masses a year), which suggests that the feedback source responsible for preventing runaway cooling in nearby cool-core clusters may not yet be fully established in SPT-CLJ2344-4243. This large star-formation rate implies that a significant fraction of the stars in the central galaxy of this cluster may form through accretion of the intracluster medium, rather than (as is currently thought) assembling entirely via mergers. © 2012 Macmillan Publishers Limited. All rights reserved.
• Mũoz, D., Marrone, D. P., Moran, J. M., & Rao, R. (2012). The circular polarization of sagittarius A* at submillimeter wavelengths. Astrophysical Journal, 745(2).
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  Abstract: We report the first detections of circularly polarized emission at submillimeter wavelengths from the compact radio source and supermassive black hole candidate SgrA* at a level of 1.2% 0.3% at 1.3 mm wavelength (230GHz) and 1.6% 0.3% at 860 μm (345GHz) with the same handedness, left circular polarization (LCP), as observed at all lower frequencies (1.4-15GHz). The observations, taken with the Submillimeter Array in multiple epochs, also show simultaneous linear polarization (LP) at both wavelengths of about 6%. These properties differ sharply from those at wavelengths longer than 1 cm (frequencies below 30GHz), where weak circular polarization (CP) (0.5%) dominates over LP, which is not detected at similar fractional limits. We describe an extensive set of tests to ensure the accuracy of our measurements. We find no CP in any other source, including the bright quasar 1924-292, which traces the same path on the sky as SgrA* and therefore should be subject to identical systematic errors originating in the instrument frame. Since a relativistic synchrotron plasma is expected to produce little CP, the observed CP is probably generated close to the event horizon by the Faraday conversion process. We use a simple approximation to show that the phase shift associated with Faraday conversion can be nearly independent of frequency, a sufficient condition to make the handedness of CP independent of frequency. Because the size of the τ = 1 surface changes by more than an order of magnitude between 1.4 and 345GHz, the magnetic field must be coherent over such scales to consistently produce LCP. To improve our understanding of the environment of SgrA* critical future measurements includes determining whether the Faraday rotation deviates from a λ 2 dependence in wavelength and whether the circular and linear components of the flux density are correlated. © 2012. The American Astronomical Society. All rights reserved.
• Sayre, J. T., Ade, P., Aird, K. A., Austermann, J. E., Beall, J. A., Becker, D., Benson, B. A., Bleem, L. E., Britton, J., Carlstrom, J. E., Chang, C. L., Cho, H. -., Crawford, T. M., Crites, A. T., Datesman, A., Haan, T. D., Dobbs, M. A., Everett, W., Ewall-Wice, A., , George, E. M., et al. (2012). Design and characterization of 90 GHz feedhorn-coupled TES polarimeter pixels in the SPTpol camera. Proceedings of SPIE - The International Society for Optical Engineering, 8452.
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  Abstract: The SPTpol camera is a two-color, polarization-sensitive bolometer receiver, and was installed on the 10 meter South Pole Telescope in January 2012. SPTpol is designed to study the faint polarization signals in the Cosmic Microwave Background, with two primary scientific goals. One is to constrain the tensor-to-scalar ratio of perturbations in the primordial plasma, and thus constrain the space of permissible inflationary models. The other is to measure the weak lensing effect of large-scale structure on CMB polarization, which can be used to constrain the sum of neutrino masses as well as other growth-related parameters. The SPTpol focal plane consists of seven 84-element monolithic arrays of 150 GHz pixels (588 total) and 180 individual 90 GHz single-pixel modules. In this paper we present the design and characterization of the 90 GHz modules. © 2012 SPIE.
• Semler, D. R., Šuhada, R., Aird, K. A., Ashby, M. L., Bautz, M., Bayliss, M., Bazin, G., Bocquet, S., Benson, B. A., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., Haan, T. D., Desai, S., , Dobbs, M. A., et al. (2012). High-redshift cool-core galaxy clusters detected via the Sunyaev-Zel'dovich effect in the south pole telescope survey. Astrophysical Journal, 761(2).
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  Abstract: We report the first investigation of cool-core properties of galaxy clusters selected via their Sunyaev-Zel'dovich (SZ) effect. We use 13 galaxy clusters uniformly selected from 178 deg2 observed with the South Pole Telescope (SPT) and followed up by the Chandra X-ray Observatory. They form an approximately mass-limited sample (>3 × 1014 M ⊙h -170) spanning redshifts 0.3 < z < 1.1. Using previously published X-ray-selected cluster samples, we compare two proxies of cool-core strength: surface brightness concentration (cSB) and cuspiness (α). We find that c SBis better constrained. We measure c SBfor the SPT sample and find several new z > 0.5 cool-core clusters, including two strong cool cores. This rules out the hypothesis that there are no z > 0.5 clusters that qualify as strong cool cores at the 5.4σ level. The fraction of strong cool-core clusters in the SPT sample in this redshift regime is between 7% and 56% (95% confidence). Although the SPT selection function is significantly different from the X-ray samples, the high-z c SBdistribution for the SPT sample is statistically consistent with that of X-ray-selected samples at both low and high redshifts. The cool-core strength is inversely correlated with the offset between the brightest cluster galaxy and the X-ray centroid, providing evidence that the dynamical state affects the cool-core strength of the cluster. Larger SZ-selected samples will be crucial in understanding the evolution of cluster cool cores over cosmic time. © 2012. The American Astronomical Society. All rights reserved..
• Shirokoff, E., Barry, P. S., Bradford, C. M., Chattopadhyay, G., Day, P., Doyle, S., Hailey-Dunsheath, S., Hollister, M. I., Kovács, A., McKenney, C., Leduc, H. G., Llombart, N., Marrone, D. P., Mauskopf, P., O'Brient, R., Padin, S., Reck, T., Swenson, L. J., & Zmuidzinas, J. (2012). MKID development for SuperSpec: An on-chip, mm-wave, filter-bank spectrometer. Proceedings of SPIE - The International Society for Optical Engineering, 8452.
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  Abstract: SuperSpec is an ultra-compact spectrometer-on-a-chip for millimeter and submillimeter wavelength astronomy. Its very small size, wide spectral bandwidth, and highly multiplexed readout will enable construction of powerful multibeam spectrometers for high-redshift observations. The spectrometer consists of a horn-coupled microstrip feedline, a bank of narrow-band superconducting resonator filters that provide spectral selectivity, and kinetic inductance detectors (KIDs) that detect the power admitted by each filter resonator. The design is realized using thin-film lithographic structures on a silicon wafer. The mm-wave microstrip feedline and spectral filters of the first prototype are designed to operate in the band from 195-310 GHz and are fabricated from niobium with at Tc of 9:2K: The KIDs are designed to operate at hundreds of MHz and are fabricated from titanium nitride with a Tc of ∼ 2 K. Radiation incident on the horn travels along the mm-wave microstrip, passes through the frequency-selective filter, and is finally absorbed by the corresponding KID where it causes a measurable shift in the resonant frequency. In this proceedings, we present the design of the KIDs employed in SuperSpec and the results of initial laboratory testing of a prototype device. We will also briefly describe the ongoing development of a demonstration instrument that will consist of two 500-channel, R=700 spectrometers, one operating in the 1-mm atmospheric window and the other covering the 650 and 850 micron bands. © 2012 SPIE.
• Song, J., Zenteno, A., Stalder, B., Desai, S., Bleem, L. E., Aird, K. A., Armstrong, R., Ashby, M. L., Bayliss, M., Bazin, G., Benson, B. A., Bertin, E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. M., Clocchiatti, A., Crawford, T. M., Crites, A. T., , Haan, T. D., et al. (2012). Redshifts, sample purity, and BCG positions for the galaxy cluster catalog from the first 720 square degrees of the south pole telescope survey. Astrophysical Journal, 761(1).
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  Abstract: We present the results of the ground- and space-based optical and near-infrared (NIR) follow-up of 224 galaxy cluster candidates detected with the Sunyaev-Zel'dovich (SZ) effect in the 720 deg 2 of the South Pole Telescope (SPT) survey completed in the 2008 and 2009 observing seasons. We use the optical/NIR data to establish whether each candidate is associated with an overdensity of galaxies and to estimate the cluster redshift. Most photometric redshifts are derived through a combination of three different cluster redshift estimators using red-sequence galaxies, resulting in an accuracy of Δz/(1 + z) = 0.017, determined through comparison with a subsample of 57 clusters for which we have spectroscopic redshifts. We successfully measure redshifts for 158 systems and present redshift lower limits for the remaining candidates. The redshift distribution of the confirmed clusters extends to z = 1.35 with a median of z med = 0.57. Approximately 18% of the sample with measured redshifts lies at z > 0.8. We estimate a lower limit to the purity of this SPT SZ-selected sample by assuming that all unconfirmed clusters are noise fluctuations in the SPT data. We show that the cumulative purity at detection significance ξ > 5(ξ > 4.5) is ≥95% (≥70%). We present the red brightest cluster galaxy (rBCG) positions for the sample and examine the offsets between the SPT candidate position and the rBCG. The radial distribution of offsets is similar to that seen in X-ray-selected cluster samples, providing no evidence that SZ-selected cluster samples include a different fraction of recent mergers from X-ray-selected cluster samples. © 2012. The American Astronomical Society. All rights reserved..
• Story, K., Leitch, E., Ade, P., Aird, K. A., Austermann, J. E., Beall, J. A., Becker, D., Bender, A. N., Benson, B. A., Bleem, L. E., Britton, J., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Cho, H. -., Crawford, T. M., Crites, A. T., Datesman, A., Haan, T. D., , Dobbs, M. A., et al. (2012). South Pole Telescope software systems: Control, monitoring, and data acquisition. Proceedings of SPIE - The International Society for Optical Engineering, 8451.
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  Abstract: We present the software system used to control and operate the South Pole Telescope. The South Pole Telescope is a 10-meter millimeter-wavelength telescope designed to measure anisotropies in the cosmic microwave background (CMB) at arcminute angular resolution. In the austral summer of 2011/12, the SPT was equipped with a new polarization-sensitive camera, which consists of 1536 transition-edge sensor bolometers. The bolometers are read out using 36 independent digital frequency multiplexing (DfMux) readout boards, each with its own embedded processors. These autonomous boards control and read out data from the focal plane with on-board software and firmware. An overall control software system running on a separate control computer controls the DfMux boards, the cryostat and all other aspects of telescope operation. This control software collects and monitors data in real-time, and stores the data to disk for transfer to the United States for analysis. © 2012 SPIE.
• Andersson, K., Benson, B. A., Ade, P. A., Aird, K. A., Armstrong, B., Bautz, M., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Crawford, T. M., Crites, A. T., Haan, T. D., Desai, S., Dobbs, M. A., Dudley, J. P., Foley, R. J., Forman, W. R., Garmire, G., , George, E. M., et al. (2011). X-ray properties of the first Sunyaev-Zel'dovich effect selected galaxy cluster sample from the South Pole Telescope. Astrophysical Journal, 738(1).
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  Abstract: We present results of X-ray observations of a sample of 15 clusters selected via their imprint on the cosmic microwave background from the thermal Sunyaev-Zel'dovich (SZ) effect. These clusters are a subset of the first SZ-selected cluster catalog, obtained from observations of 178 deg2 of sky surveyed by the South Pole Telescope (SPT). Using X-ray observations with Chandra and XMM-Newton, we estimate the temperature, TX , and mass, Mg , of the intracluster medium within r 500 for each cluster. From these, we calculate YX = MgTX and estimate the total cluster mass using an M 500-YX scaling relation measured from previous X-ray studies. The integrated Comptonization, Y SZ, is derived from the SZ measurements, using additional information from the X-ray-measured gas density profiles and a universal temperature profile. We calculate scaling relations between the X-ray and SZ observables and find results generally consistent with other measurements and the expectations from simple self-similar behavior. Specifically, we fit a Y SZ-YX relation and find a normalization of 0.82 ± 0.07, marginally consistent with the predicted ratio of Y SZ/Y X = 0.91 ± 0.01 that would be expected from the density and temperature models used in this work. Using the YX -derived mass estimates, we fit a Y SZ-M 500 relation and find a slope consistent with the self-similar expectation of Y SZM 5/3 with a normalization consistent with predictions from other X-ray studies. We find that the SZ mass estimates, derived from cosmological simulations of the SPT survey, are lower by a factor of 0.78 ± 0.06 relative to the X-ray mass estimates. This offset is at a level of 1.3σ when considering the 15% systematic uncertainty for the simulation-based SZ masses. Overall, the X-ray measurements confirm that the scaling relations of the SZ-selected clusters are consistent with the properties of other X-ray-selected samples of massive clusters, even allowing for the broad redshift range (0.29 < z < 1.08) of the sample. © 2011. The American Astronomical Society. All rights reserved..
• Enoch, M. L., Corder, S., Duchêne, G., Bock, D. C., Bolatto, A. D., Culverhouse, T. L., Kwon, W., Lamb, J. W., Leitch, E. M., Marrone, D. P., Muchovej, S. J., Pérez, L. M., Scott, S. L., Teuben, P. J., C., M., & Zauderer, B. A. (2011). Disk and envelope structure in class 0 protostars. II. High-resolution millimeter mapping of the Serpens sample. Astrophysical Journal, Supplement Series, 195(2).
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  Abstract: We present high-resolution CARMA 230GHz continuum imaging of nine deeply embedded protostars in the Serpens Molecular Cloud, including six of the nine known Class 0 protostars in Serpens. This work is part of a program to characterize disk and envelope properties for a complete sample of Class 0 protostars in nearby low-mass star-forming regions. Here, we present CARMA maps and visibility amplitudes as a function of uv-distance for the Serpens sample. Observations are made in the B, C, D, and E antenna configurations, with B configuration observations utilizing the CARMA Paired Antenna Calibration System. Combining data from multiple configurations provides excellent uv-coverage (4-500kλ), allowing us to trace spatial scales from 10 2 to 104AU. We find evidence for compact disk components in all of the observed Class 0 protostars, suggesting that disks form at very early times (t < 0.2Myr) in Serpens. We make a first estimate of disk masses using the flux at 50kλ, where the contribution from the envelope should be negligible, assuming an unresolved disk. The resulting disk masses range from 0.04 M⊙ to 1.7 M⊙, with a mean of approximately 0.2 M⊙. Our high-resolution maps are also sensitive to binary or multiple sources with separations ≳ 250AU, but significant evidence of multiplicity on scales
• Foley, R. J., Andersson, K., Bazin, G., Haan, T. D., Ruel, J., Ade, P. A., Aird, K. A., Armstrong, R., Ashby, M. L., Bautz, M., Benson, B. A., Bleem, L. E., Bonamente, M., Brodwin, M., Carlstrom, J. E., Chang, C. L., Clocchiatti, A., Crawford, T. M., Crites, A. T., , Desai, S., et al. (2011). Discovery and cosmological implications of SPT-CL J2106-5844, the most massive known cluster at z>1. Astrophysical Journal, 731(2).
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  Abstract: Using the South Pole Telescope (SPT), we have discovered the most massive known galaxy cluster at z>1, SPT-CL J2106-5844. In addition to producing a strong Sunyaev-Zel'dovich (SZ) effect signal, this system is a luminous X-ray source and its numerous constituent galaxies display spatial and color clustering, all indicating the presence of a massive galaxy cluster. Very Large Telescope and Magellan spectroscopy of 18 member galaxies shows that the cluster is at z = 1.132+0.002-0.003. Chandra observations obtained through a combined HRC-ACIS GTO program reveal an X-ray spectrum with an Fe K line redshifted by z = 1.18 ± 0.03. These redshifts are consistent with the galaxy colors found in optical, near-infrared, and mid-infrared imaging. SPT-CL J2106-5844 displays extreme X-ray properties for a cluster having a core-excluded temperature of TX = 11.0 +2.6-1.9keV and a luminosity (within r 500) of LX (0.5-2.0 keV) = (13.9 ± 1.0) × 10 44ergs-1. The combined mass estimate from measurements of the SZ effect and X-ray data is M 200 = (1.27 ± 0.21) × 1015h -170 M ⊙. The discovery of such a massive gravitationally collapsed system at high redshift provides an interesting laboratory for galaxy formation and evolution, and is a probe of extreme perturbations of the primordial matter density field. We discuss the latter, determining that, under the assumption of ΛCDM cosmology with only Gaussian perturbations, there is only a 7% chance of finding a galaxy cluster similar to SPT-CL J2106-5844 in the 2500deg2 SPT survey region and that only one such galaxy cluster is expected in the entire sky. © 2011. The American Astronomical Society. All rights reserved.
• Gralla, M. B., Sharon, K., Gladders, M. D., Marrone, D. P., Barrientos, L. F., Bayliss, M., Bonamente, M., Bulbul, E., Carlstrom, J. E., Culverhouse, T., Gilbank, D. G., Greer, C., Hasler, N., Hawkins, D., Hennessy, R., Joy, M., Koester, B., Lamb, J., Leitch, E., , Miller, A., et al. (2011). Sunyaev-zel'dovich effect observations of strong lensing galaxy clusters: Probing the overconcentration problem. Astrophysical Journal, 737(2).
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  Abstract: We have measured the Sunyaev-Zel'dovich (SZ) effect for a sample of 10 strong lensing selected galaxy clusters using the Sunyaev-Zel'dovich Array (SZA). The SZA is sensitive to structures on spatial scales of a few arcminutes, while the strong lensing mass modeling constrains the mass at small scales (typically
• Muchovej, S., Leitch, E., Carlstrom, J. E., Culverhouse, T., Greer, C., Hawkins, D., Hennessy, R., Joy, M., Lamb, J., Loh, M., Marrone, D. P., Miller, A., Mroczkowski, T., Pryke, C., Sharp, M., & Woody, D. (2011). Cosmological constraints from a 31 GHz sky survey with the Sunyaev-Zel'dovich array. Astrophysical Journal, 732(1).
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  Abstract: We present the results of an analysis of 4.4 deg2 selected from a 6.1 deg2 survey for clusters of galaxies via their Sunyaev-Zel'dovich effect at 31 GHz. From late 2005 to mid 2007, the Sunyaev-Zel'dovich Array observed four fields of roughly 1.5 deg2 each. One of the fields shows evidence for significant diffuse Galactic emission, and is therefore excised from this analysis. We estimate the cluster detectability for the survey using mock observations of simulations of clusters of galaxies and determine that, at intermediate redshifts (z ∼ 0.8), the survey is 50% complete to a limiting mass (M200ρ̄) of ∼6.0 × 1014 M⊙, with the mass limit decreasing at higher redshifts. We detect no clusters at a significance greater than five times the rms noise level in the maps, and place an upper limit on σ8, the amplitude of mass density fluctuations on a scale of 8 h -1 Mpc, of 0.84 + 0.04 + 0.04 at 95% confidence, where the first uncertainty reflects an estimate of additional sample variance due to non-Gaussianity in the distribution of clusters and the second reflects calibration and systematic effects. This result is consistent with estimates from other cluster surveys and cosmic microwave background anisotropy experiments. © 2011. The American Astronomical Society. All rights reserved.
• Rao, R., Girart, J. -., & Marrone, D. P. (2011). Submillimeter array observations of magnetic fields in star forming regions. Proceedings of the International Astronomical Union, 6(S270), 103-106.
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  Abstract: There have been a number of theoretical and computational models which state that magnetic fields play an important role in the process of star formation. Competing theories instead postulate that it is turbulence which is dominant and magnetic fields are weak. The recent installation of a polarimetry system at the Submillimeter Array (SMA) has enabled us to conduct observations that could potentially distinguish between the two theories. Some of the nearby low mass star forming regions show hour-glass shaped magnetic field structures that are consistent with theoretical models in which the magnetic field plays a dominant role. However, there are other similar regions where no significant polarization is detected. Future polarimetry observations made by the Submillimeter Array should be able to increase the sample of observed regions. These measurements will allow us to address observationally the important question of the role of magnetic fields and/or turbulence in the process of star formation. © 2011 International Astronomical Union.
• Story, K., Aird, K. A., Andersson, K., Armstrong, R., Bazin, G., Benson, B. A., Bleem, L. E., Bonamente, M., Brodwin, M., Carlstrom, J. E., Chang, C. L., Clocchiatti, A., Crawford, T. M., Crites, A. T., Haan, T. D., Desai, S., Dobbs, M. A., Dudley, J. P., Foley, R. J., , George, E. M., et al. (2011). South pole telescope detections of the previously unconfirmed Planck Early Sunyaev-Zel'dovich clusters in the southern hemisphere. Astrophysical Journal Letters, 735(2).
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  Abstract: We present South Pole Telescope (SPT) observations of the five galaxy cluster candidates in the southern hemisphere which were reported as unconfirmed in the Planck Early Sunyaev-Zel'dovich (ESZ) sample. One cluster candidate, PLCKESZ G255.62-46.16, is located in the 2500deg2 SPT SZ survey region and was reported previously as SPT-CL J0411-4819. For the remaining four candidates, which are located outside of the SPT SZ survey region, we performed short, dedicated SPT observations. Each of these four candidates was strongly detected in maps made from these observations, with signal-to-noise ratios ranging from 6.3 to 13.8. We have observed these four candidates on the Magellan-Baade telescope and used these data to estimate cluster redshifts from the red sequence. Resulting redshifts range from 0.24 to 0.46. We report measurements of Y 075, the integrated Comptonization within a 075 radius, for all five candidates. We also report X-ray luminosities calculated from ROSAT All-Sky Survey catalog counts, as well as optical and improved SZ coordinates for each candidate. The combination of SPT SZ measurements, optical red-sequence measurements, and X-ray luminosity estimates demonstrates that these five Planck ESZ cluster candidates do indeed correspond to real galaxy clusters with redshifts and observable properties consistent with the rest of the ESZ sample. © 2011. The American Astronomical Society. All rights reserved.
• Williamson, R., Benson, B. A., High, F. W., Vanderlinde, K., Ade, P. A., Aird, K. A., Andersson, K., Armstrong, R., Ashby, M. L., Bautz, M., Bazin, G., Bertin, E., Bleem, L. E., Bonamente, M., Brodwin, M., Carlstrom, J. E., Chang, C. L., Chapman, S. C., Clocchiatti, A., , Crawford, T. M., et al. (2011). A Sunyaev-Zel'dovich-selected sample of the most massive galaxy clusters in the 2500 deg² South Pole telescope survey. Astrophysical Journal, 738(2).
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  Abstract: The South Pole Telescope (SPT) is currently surveying 2500deg2 of the southern sky to detect massive galaxy clusters out to the epoch of their formation using the Sunyaev-Zel'dovich (SZ) effect. This paper presents a catalog of the 26 most significant SZ cluster detections in the full survey region. The catalog includes 14 clusters which have been previously identified and 12 that are new discoveries. These clusters were identified in fields observed to two differing noise depths: 1500deg2 at the final SPT survey depth of 18μK arcmin at 150GHz and 1000deg2 at a depth of 54μK arcmin. Clusters were selected on the basis of their SZ signal-to-noise ratio (S/N) in SPT maps, a quantity which has been demonstrated to correlate tightly with cluster mass. The S/N thresholds were chosen to achieve a comparable mass selection across survey fields of both depths. Cluster redshifts were obtained with optical and infrared imaging and spectroscopy from a variety of ground- and space-based facilities. The redshifts range from 0.098 ≤ z ≤ 1.132 with a median of z med = 0.40. The measured SZ S/N and redshifts lead to unbiased mass estimates ranging from 9.8 × 10 14 M® h -170 ≤ M 200(ρ mean) ≤ 3.1 × 1015 M® h -170. Based on the SZ mass estimates, we find that none of the clusters are individually in significant tension with the ΛCDM cosmological model. We also test for evidence of non-Gaussianity based on the cluster sample and find the data show no preference for non-Gaussian perturbations. © 2011. The American Astronomical Society. All rights reserved.
• Brodwin, M., Ruel, J., Ade, P. A., Aird, K. A., Andersson, K., Ashby, M. L., Bautz, M., Bazin, G., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Crawford, T. M., Crites, A. T., Haan, T. D., Desai, S., Dobbs, M. A., Dudley, J. P., Fazio, G. G., , Foley, R. J., et al. (2010). SPT-CL J0546-5345: A massive z > 1 galaxy cluster selected via the Sunyaev-Zel'dovich Effect with the South Pole Telescope. Astrophysical Journal Letters, 721(1), 90-97.
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  Abstract: We report the spectroscopic confirmation of SPT-CL J0546-5345 at (z) = 1.067. To date this is the most distant cluster to be spectroscopically confirmed from the 2008 South Pole Telescope (SPT) catalog, and indeed the first z > 1 cluster discovered by the Sunyaev-Zel'dovich Effect (SZE). We identify 21 secure spectroscopic members within 0.9 Mpc of the SPT cluster position, 18 of which are quiescent, early-type galaxies. From these quiescent galaxies we obtain a velocity dispersion of 1179-167+232 km s -1, ranking SPT-CL J0546-5345 as the most dynamically massive cluster yet discovered at z > 1. Assuming that SPT-CL J0546-5345 is virialized, this implies a dynamical mass of M200 = 1.0-0.4+0.6×1015M⊙, in agreement with the X-ray and SZE mass measurements. Combining masses from several independent measures leads to a best-estimate mass of M200 = (7.95 ± 0.92) × 1014M⊙. The spectroscopic confirmation of SPT-CL J0546-5345, discovered in the wide-angle, mass-selected SPT cluster survey, marks the onset of the high-redshift SZE-selected galaxy cluster era. © 2010. The American Astronomical Society. All rights reserved.
• Culverhouse, T. L., Bonamente, M., Bulbul, E., Carlstrom, J. E., Gralla, M. B., Greer, C., Hasler, N., Hawkins, D., Hennessy, R., Jetha, N. N., Joy, M., Lamb, J. W., Leitch, E. M., Marrone, D. P., Miller, A., Mroczkowski, T., Muchovej, S., Pryke, C., Sharp, M., , Woody, D., et al. (2010). Galaxy clusters at z ≥ 1: Gas constraints from the Sunyaev-Zel'dovich array. Astrophysical Journal Letters, 723(1 PART 2), L78-L83.
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  Abstract: We present gas constraints from Sunyaev-Zel'dovich (SZ) effect measurements in a sample of 11 X-ray and infrared (IR) selected galaxy clusters at z ≥1, using data from the Sunyaev-Zel'dovich Array (SZA). The cylindrically integrated Compton-y parameter, Y, is calculated by fitting the data to a two-parameter gas pressure profile. Where possible, we also determine the temperature of the hot intracluster plasma from Chandra and XMM-Newton data and constrain the gas mass within the same aperture (r2500) as Y. The SZ effect is detected in the clusters for which the X-ray data indicate gas masses above ∼10 13M⊙, including XMMU J2235-2557 at redshift z = 1.39, which to date is one of the most distant clusters detected using the SZ effect. None of the IR-selected targets are detected by the SZA measurements, indicating low gas masses for these objects. For these and the four other undetected clusters, we quote upper limits on Y andMgas,SZ, with the latter derived from scaling relations calibrated with lower redshift clusters. We compare the constraints on Y and X-ray-derived gas mass Mgas,X-ray to self-similar scaling relations between these observables determined from observations of lower redshift clusters, finding consistency given the measurement error. © 2010. The American Astronomical Society. All rights reserved.
• High, F. W., Stalder, B., Song, J., Ade, P. A., Aird, K. A., Allam, S. S., Armstrong, R., Barkhouse, W. A., Benson, B. A., Bertin, E., Bhattacharya, S., Bleem, L. E., Brodwin, M., Buckley-Geer, E., Carlstrom, J. E., Challis, P., Chang, C. L., Crawford, T. M., Crites, A. T., , Haan, T. D., et al. (2010). Optical redshift and richness estimates for galaxy clusters selected with the Sunyaev-Zel'dovich effect from 2008 South Pole Telescope observations. Astrophysical Journal Letters, 723(2), 1736-1747.
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  Abstract: We present redshifts and optical richness properties of 21 galaxy clusters uniformly selected by their Sunyaev-Zel'dovich (SZ) signature. These clusters, plus an additional, unconfirmed candidate, were detected in a 178 deg 2 area surveyed by the South Pole Telescope (SPT) in 2008. Using griz imaging from the Blanco Cosmology Survey and from pointed Magellan telescope observations, as well as spectroscopy using Magellan facilities, we confirm the existence of clustered red-sequence galaxies, report red-sequence photometric redshifts, present spectroscopic redshifts for a subsample, and derive R 200 radii and M200 masses from optical richness. The clusters span redshifts from 0.15 to greater than 1, with a median redshift of 0.74; three clusters are estimated to be at z > 1. Redshifts inferred from mean red-sequence colors exhibit 2% rms scatter in σz/(1 + z) with respect to the spectroscopic subsample for z > 1. We show that the M200 cluster masses derived from optical richness correlate with masses derived from SPT data and agree with previously derived scaling relations to within the uncertainties. Optical and infrared imaging is an efficient means of cluster identification and redshift estimation in large SZ surveys, and exploiting the same data for richness measurements, as we have done, will be useful for constraining cluster masses and radii for large samples in cosmological analysis. © 2010. The American Astronomical Society.
• Muchovej, S., Leitch, E., Carlstrom, J. E., Culverhouse, T., Greer, C., Hawkins, D., Hennessy, R., Joy, M., Lamb, J., Loh, M., Marrone, D. P., Miller, A., Mroczkowski, T., Pryke, C., Sharp, M., & Woody, D. (2010). Radio sources from A 31 GHz sky survey with the sunyaev-zel'dovich array. Astrophysical Journal Letters, 716(1), 521-529.
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  Abstract: We present the first sample of 31 GHz selected sources to flux levels of 1 mJy. From late 2005 to mid-2007, the Sunyaev-Zel'dovich Array observed 7.7 deg2 of the sky at 31 GHz to a median rms of 0.18 mJy beam -1. We identify 209 sources at greater than 5σ significance in the 31 GHz maps, ranging in flux from 0.7mJy to 200 mJy. Archival NVSS data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. We determine the maximum-likelihood integrated source count to be N(>S) = (27.2 ± 2.5)deg-2 × (S mJy)-1.18 ± 0.12 over the flux range 0.7-15 mJy. This result is significantly higher than predictions based on 1.4 GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4 GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, we derive an overdensity of 6.8 4.4, relative to field sources. © 2010. The American Astronomical Society. All rights reserved.
• Plagge, T., Benson, B. A., Ade, P. A., Aird, K. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Cho, H. -., Crawford, T. M., Crites, A. T., Haan, T. D., Dobbs, M. A., George, E. M., Hall, N. R., Halverson, N. W., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Joy, M., , Keisler, R., et al. (2010). Sunyaev-zel'dovich cluster profiles measured with the South Pole telescope. Astrophysical Journal Letters, 716(2), 1118-1135.
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  Abstract: We present Sunyaev-Zel'dovich (SZ) measurements of 15 massive X-ray-selected galaxy clusters obtained with the South Pole Telescope (SPT). The SZ cluster signals are measured at 150 GHz, and concurrent 220GHz data are used to reduce astrophysical contamination. Radial profiles are computed using a technique that takes into account the effects of the beams and filtering. In several clusters, significant SZ decrements are detected out to a substantial fraction of the virial radius. The profiles are fit to the β-model and to a generalized Navarro-Frenk-White (NFW) pressure profile, and are scaled and stacked to probe their average behavior. We find model parameters that are consistent with previous studies: β = 0.86 and r core/r 500 = 0.20 for the β-model, and (αn, βn, γn, c 500) = (1.0, 5.5, 0.5, 1.0) for the generalized NFW model. Both models fit the SPT data comparably well, and both are consistent with the average SZ profile out to beyond r 500. The integrated Compton-y parameter Y SZ is computed for each cluster using both model-dependent and model-independent techniques, and the results are compared to X-ray estimates of cluster parameters. We find that Y SZ scales with YX and gas mass with low scatter. Since these observables have been found to scale with total mass, our results point to a tight mass-observable relation for the SPT cluster survey. © 2010. The American Astronomical Society. All rights reserved.
• Pérez, L. M., Lamb, J. W., Woody, D. P., Carpenter, J. M., Zauderer, B. A., Isella, A., Bock, D. C., Bolatto, A. D., Carlstrom, J., Culverhouse, T. L., Joy, M., Kwon, W., Leitch, E. M., Marrone, D. P., Muchovej, S. J., Plambeck, R. L., Scott, S. L., Teuben, P. J., & C., M. (2010). Atmospheric phase correction using CARMA-PACS: High angular resolution observations of the FU Orionis star PP 13S. Astrophysical Journal Letters, 724(1), 493-501.
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  Abstract: We present 0′′15 resolution observations of the 227 GHz continuum emission from the circumstellar disk around the FU Orionis star PP 13S*. The data were obtained with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) Paired Antenna Calibration System (C-PACS), which measures and corrects the atmospheric delay fluctuations on the longest baselines of the array in order to improve the sensitivity and angular resolution of the observations. A description of the C-PACS technique and the data reduction procedures are presented. C-PACS was applied to CARMA observations of PP 13S*, which led to a factor of 1.6 increase in the observed peak flux of the source, a 36% reduction in the noise of the image, and a 52% decrease in the measured size of the source major axis. The calibrated complex visibilities were fitted with a theoretical disk model to constrain the disk surface density. The total disk mass from the best-fit model corresponds to 0.06 M⊙, which is larger than the median mass of a disk around a classical T Tauri star. The disk is optically thick at a wavelength of 1.3 mm for orbital radii less than 48 AU. At larger radii, the inferred surface density of the PP 13S* disk is an order of magnitude lower than that needed to develop a gravitational instability.
• Pérez, L. M., Lamb, J. W., Woody, D. P., Zauderer, B. A., Carpenter, J. M., Bolatto, A. D., Leitch, E. M., Marrone, D. P., Mundy, L. G., Plambeck, R. L., Teuben, P. J., & C., M. (2010). Atmospheric phase correction using the CARMA paired antennas calibration system. Proceedings of SPIE - The International Society for Optical Engineering, 7733(PART 1).
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  Abstract: High angular resolution observations are essential to understand a variety of astrophysical phenomena. The resolution of millimeter wave interferometers is limited by large and rapid differential atmospheric delay fluctuations. At the Combined Array for Research in Millimeter-wave Astronomy (CARMA) we have employed a Paired Antenna Calibration System (C-PACS) for atmospheric phase compensation in the extended array configurations (up to 2 km baselines). We present a description of C-PACS and its application. We also present successful atmospheric delay corrections applied to science observations with dramatic improvements in sensitivity and angular resolution. © 2010 SPIE.
• Sharp, M. K., Marrone, D. P., Carlstrom, J. E., Culverhouse, T., Greer, C., Hawkins, D., Hennessy, R., Joy, M., Lamb, J. W., Leitch, E. M., Loh, M., Miller, A., Mroczkowski, T., Muchovej, S., Pryke, C., & Woody, D. (2010). A measurement of arcminute anisotropy in the cosmic microwave background with the sunyaev-zel'dovich array. Astrophysical Journal Letters, 713(1), 82-89.
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  Abstract: We present 30 GHz measurements of the angular power spectrum of the cosmic microwave background (CMB) obtained with the Sunyaev-Zel'dovich Array. The measurements are sensitive to arcminute angular scales, where secondary anisotropy from the Sunyaev-Zel'dovich effect (SZE) is expected to dominate. For a broad bin centered at multipole 4066, we find 67+77-50 μK2; of which 26 ± 5 μK2 is the expected contribution from primary CMB anisotropy and 80 ± 54 μK2 is the expected contribution from undetected radio sources. These results imply an upper limit of 155 μK2 (95% CL) on the secondary contribution to the anisotropy in our maps. This level of SZE anisotropy power is consistent with expectations based on recent determinations of the normalization of the matter power spectrum, i.e., σ ∼ 8 0.8. © 2010. The American Astronomical Society. All rights reserved.
• Vanderlinde, K., Crawford, T. M., Haan, T. D., Dudley, J. P., Shaw, L., Ade, P. A., Aird, K. A., Benson, B. A., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Crites, A. T., Desai, S., Dobbs, M. A., Foley, R. J., George, E. M., Gladders, M. D., Hall, N. R., , Halverson, N. W., et al. (2010). Galaxy clusters selected with the Sunyaev-Zel'dovich effect from 2008 South Pole Telescope observations. Astrophysical Journal Letters, 722(2), 1180-1196.
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  Abstract: We present a detection-significance-limited catalog of 21 Sunyaev-Zel'dovich-selected galaxy clusters. These clusters, along with one unconfirmed candidate, were identified in 178 deg2 of sky surveyed in 2008 by the South Pole Telescope (SPT) to a depth of 18 μK arcmin at 150 GHz. Optical imaging from the Blanco Cosmology Survey (BCS) and Magellan telescopes provided photometric (and in some cases spectroscopic) redshift estimates, with catalog redshifts ranging from z = 0.15 to z > 1, with a median z = 0.74. Of the 21 confirmed galaxy clusters, 3 were previously identified as Abell clusters, 3 were presented as SPT discoveries in Staniszewski et al., and 3 were first identified in a recent analysis of BCS data by Menanteau et al.; the remaining 12 clusters are presented for the first time in this work. Simulated observations of the SPT fields predict the sample to be nearly 100% complete above a mass threshold of M200 ≈5× 1014 M⊙ h-1 at z = 0.6. This completeness threshold pushes to lower mass with increasing redshift, dropping to ∼4 × 1014 M⊙ h-1 at z = 1. The size and redshift distribution ofthis catalog are in good agreement with expectations based on our current understanding of galaxy clusters and cosmology. In combination with other cosmological probes, we use this cluster catalog to improve estimates of cosmological parameters. Assuming a standard spatially flat wCDM cosmological model, the addition of our catalog to the WMAP seven-year results yields σ8 = 0.81 ±0.09 and w = -1.07 ±0.29, a ∼50% improvement in precision on both parameters over WMAP7 alone. © 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A.
• Vieira, J. D., Crawford, T. M., Switzer, E. R., Ade, P. A., Aird, K. A., Ashby, M. L., Benson, B. A., Bleem, L. E., Brodwin, M., Carlstrom, J. E., Chang, C. L., Cho, H. -., Crites, A. T., Haan, T. D., Dobbs, M. A., Everett, W., George, E. M., Gladders, M., Hall, N. R., , Halverson, N. W., et al. (2010). Extragalactic millimeter-wave sources in South Pole Telescope survey data: Source counts, catalog, and statistics for an 87 square-degree field. Astrophysical Journal Letters, 719(1), 763-783.
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  Abstract: We report the results of an 87 deg2 point-source survey centered at R.A. 5h30m, decl. -55° taken with the South Pole Telescope at 1.4 and 2.0 mm wavelengths with arcminute resolution and milli-Jansky depth. Based on the ratio of flux in the two bands, we separate the detected sources into two populations, one consistent with synchrotron emission from active galactic nuclei and the other consistent with thermal emission from dust. We present source counts for each population from 11 to 640 mJy at 1.4 mm and from 4.4 to 800mJy at 2.0 mm. The 2.0 mm counts are dominated by synchrotron-dominated sources across our reported flux range; the 1.4 mm counts are dominated by synchrotron-dominated sources above ∼15 mJy and by dust-dominated sources below that flux level.We detect 141 synchrotron-dominated sources and 47 dust-dominated sources at signal-to-noise ratio S/N > 4.5 in at least one band. All of the most significantly detected members of the synchrotron-dominated population are associated with sources in previously published radio catalogs. Some of the dust-dominated sources are associated with nearby (z ≪ 1) galaxies whose dust emission is also detected by the Infrared Astronomy Satellite. However, most of the bright, dust-dominated sources have no counterparts in any existing catalogs.We argue that these sources represent the rarest and brightestmembers of the population commonly referred to as submillimeter galaxies (SMGs). Because these sources are selected at longer wavelengths than in typical SMG surveys, they are expected to have a higher mean redshift distribution and may provide a new window on galaxy formation in the early universe.
• Zhang, Y., Okabe, N., Finoguenov, A., Smith, G. P., Piffaretti, R., Valdarnini, R., Babul, A., Evrard, A. E., Mazzotta, P., J., A., & Marrone, D. P. (2010). LoCuSS: A comparison of cluster mass measurements from XMM-Newton and subaru - Testing deviation from hydrostatic equilibrium and non-thermal pressure support. Astrophysical Journal Letters, 711(2), 1033-1043.
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  Abstract: We compare X-ray hydrostatic and weak-lensing mass estimates for a sample of 12 clusters that have been observed with both XMM-Newton and Subaru. At an over-density of Δ = 500, we obtain 1 - M X/M WL = 0.01 ± 0.07 for the whole sample. We also divided the sample into undisturbed and disturbed sub-samples based on quantitative X-ray morphologies using asymmetry and fluctuation parameters, obtaining 1 - M X/M WL = 0.09 ± 0.06 and -0.06 ± 0.12 for the undisturbed and disturbed clusters, respectively. In addition to non-thermal pressure support, there may be a competing effect associated with adiabatic compression and/or shock heating which leads to overestimate of X-ray hydrostatic masses for disturbed clusters, for example, in the famous merging cluster A1914. Despite the modest statistical significance of the mass discrepancy, on average, in the undisturbed clusters, we detect a clear trend of improving agreement between M X and M WL as a function of increasing over-density M X/MWL = (0.908 ± 0.004) + (0.187 ± 0.010) ·log10(δ/500). . We also examine the gas mass fractions, f gas = M gas/M WL, finding that they are an increasing function of cluster radius, with no dependence on dynamical state, in agreement with predictions from numerical simulations. Overall, our results demonstrate that XMM-Newton and Subaru are a powerful combination for calibrating systematic uncertainties in cluster mass measurements. © 2010. The American Astronomical Society.
• Zhao, J., Blundell, R., Moran, J. M., Downes, D., Schuster, K. F., & Marrone, D. P. (2010). The high-density ionized gas in the central parsec of the galaxy. Astrophysical Journal Letters, 723(2), 1097-1109.
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  Abstract: We report a study of the H30α line emission at 1.3 mm from the region around Sgr A* made with the Submillimeter Array at a resolution of 2″ over a field of 60″ (2 pc) and a velocity range of -360 to +345 km s-1. This field encompasses most of the Galactic center's "minispiral." With an isothermal homogeneous H II model, we determined the physical conditions of the ionized gas at specific locations in the Northern and Eastern Arms from the H30α line data along with Very Large Array data from the H92α line at 3.6 cm and from the radio continuum emission at 1.3 cm. The typical electron density and kinetic temperature in the minispiral arms are 3-21 × 104 cm-3 and 5000-13,000 K, respectively. The H30α and H92α line profiles are broadened due to the large velocity shear within and along the beam produced by dynamical motions in the strong gravitational field near Sgr A*. We constructed a threedimensional model of the minispiral using the orbital parameters derived under the assumptions that the gas flows are in Keplerian motion. The gas in the Eastern Arm appears to collide with the Northern Arm flow in the "Bar" region, which is located 0.1-0.2 pc south of and behind Sgr A*. Finally, a total Lyman continuum flux of 3 × 1050 photons s-1 is inferred from the assumption that the gas is photoionized and the ionizing photons for the high-density gas in the minispiral arms are from external sources, which is equivalent to ∼250 O9-type zero-age-main-sequence stars. © 2010. The American Astronomical Society.
• Eckart, A., Baganoff, F. K., Morris, M. R., Kunneriath, D., Zamaninasab, M., Witzel, G., Schödel, R., García-Marín, M., Meyer, L., Bower, G. C., Marrone, D., Bautz, M. W., Brandt, W. N., Garmire, G. P., Ricker, G. R., Straubmeier, C., Roberts, D. A., Muzic, K., Mauerhan, J., & Zensus, A. (2009). Modeling mm- to X-ray flare emission from sagittarius A. Astronomy and Astrophysics, 500(3), 935-946.
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  Abstract: Context. We report on new modeling results based on the mm- to X-ray emission of the SgrA* counterpart associated with the massive ∼4×106 Mȯ black hole at the Galactic Center.Aims. We investigate the physical processes responsible for the variable emission from SgrA*. Methods. Our modeling is based on simultaneous observations carried out on 07 July, 2004, using the NACO adaptive optics (AO) instrument at the European Southern Observatory's Very Large Telescope*and the ACIS-I instrument aboard the Chandra X-ray Observatory as well as the Submillimeter Array SMA**on Mauna Kea, Hawaii, and the Very Large Array***in New Mexico. Results. The observations revealed several flare events in all wavelength domains. Here we show that the flare emission can be described with a combination of a synchrotron self-Compton (SSC) model followed by an adiabatic expansion of the source components. The SSC emission at NIR and X-ray wavelengths involves up-scattered sub-millimeter photons from a compact source component. At the start of the flare, spectra of these components peak at frequencies between several 100 GHz and 2 THz. The adiabatic expansion then accounts for the variable emission observed at sub-mm/mm wavelengths. The derived physical quantities that describe the flare emission give a blob expansion speed of vexp ∼ 0.005 c, magnetic field of B around 60 G or less and spectral indices of α = 0.8 to 1.4, corresponding to a particle spectral index p ∼2.6 to 3.8. Conclusions. A combined SSC and adiabatic expansion model can fully account for the observed flare flux densities and delay times covering the spectral range from the X-ray to the mm-radio domain. The derived model parameters suggest that the adiabatic expansion takes place in source components that have a bulk motion larger than vexp or the expanding material contributes to a corona or disk, confined to the immediate surroundings of SgrA*. © 2009 ESO.
• Marrone, D. P., Smith, G. P., Richard, J., Joy, M., Bonamente, M., Hasler, N., Hamilton-Morris, V., Kneib, J., Culverhouse, T., Carlstrom, J. E., Greer, C., Hawkins, D., Hennessy, R., Lamb, J. W., Leitch, E. M., Loh, M., Miller, A., Mroczkowski, T., Muchovej, S., , Pryke, C., et al. (2009). LoCuSS: A comparison of sunyaev-zel'dovich effect and gravitational-lensing measurements of galaxy clusters. Astrophysical Journal Letters, 701(2 PART 2), L114-L118.
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  Abstract: We present the first measurement of the relationship between the Sunyaev-Zel'dovich effect (SZE) signal and the mass of galaxy clusters that uses gravitational lensing to measure cluster mass, based on 14 X-ray luminous clusters at z ≃ 0.2 from the Local Cluster Substructure Survey. We measure the integrated Compton y-parameter, Y, and total projected mass of the clusters (M GL) within a projected clustercentric radius of 350kpc, corresponding to mean overdensities of 4000-8000 relative to the critical density. We find self-similar scaling between M GL and Y, with a scatter in mass at fixed Y of 32%. This scatter exceeds that predicted from numerical cluster simulations, however, it is smaller than comparable measurements of the scatter in mass at fixed TX . We also find no evidence of segregation in Y between disturbed and undisturbed clusters, as had been seen with TX on the same physical scales. We compare our scaling relation to the Bonamente et al. relation based on mass measurements that assume hydrostatic equilibrium, finding no evidence for a hydrostatic mass bias in cluster cores (M GL = 0.98 ± 0.13 M HSE), consistent with both predictions from numerical simulations and lensing/X-ray-based measurements of mass-observable scaling relations at larger radii. Overall our results suggest that the SZE may be less sensitive than X-ray observations to the details of cluster physics in cluster cores. © 2009. The American Astronomical Society.
• Mroczkowski, T., Bonamente, M., Carlstrom, J. E., Culverhouse, T. L., Greer, C., Hawkins, D., Hennessy, R., Joy, M., Lamb, J. W., Leitch, E. M., Loh, M., Maughan, B., Marrone, D. P., Miller, A., Muchovej, S., Nagai, D., Pryke, C., Sharp, M., & Woody, D. (2009). Application of a self-similar pressure profile to sunyaev-zel'dovich effect data from galaxy clusters. Astrophysical Journal Letters, 694(2), 1034-1044.
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  Abstract: We investigate the utility of a new, self-similar pressure profile for fitting Sunyaev-Zel'dovich (SZ) effect observations of galaxy clusters. Current SZ imaging instruments-such as the Sunyaev-Zel'dovich Array (SZA)-are capable of probing clusters over a large range in a physical scale. A model is therefore required that can accurately describe a cluster's pressure profile over a broad range of radii from the core of the cluster out to a significant fraction of the virial radius. In the analysis presented here, we fit a radial pressure profile derived from simulations and detailed X-ray analysis of relaxed clusters to SZA observations of three clusters with exceptionally high-quality X-ray data: A1835, A1914, and CL J1226.9+3332. From the joint analysis of the SZ and X-ray data, we derive physical properties such as gas mass, total mass, gas fraction and the intrinsic, integrated Compton y-parameter. We find that parameters derived from the joint fit to the SZ and X-ray data agree well with a detailed, independent X-ray-only analysis of the same clusters. In particular, we find that, when combined with X-ray imaging data, this new pressure profile yields an independent electron radial temperature profile that is in good agreement with spectroscopic X-ray measurements. © 2009. The American Astronomical Society. All rights reserved.
• Rao, R., Girart, J. M., Marrone, D. P., Lai, S., & Schnee, S. (2009). IRAS 16293: A "magnetic" tale of two cores. Astrophysical Journal Letters, 707(2), 921-935.
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  Abstract: We present polarization observations of the dust continuum emission from the young star-forming region IRAS 16293. These observations of IRAS 16293, which is a binary system, were conducted by the Submillimeter Array at an observing frequency of 341.5GHz (λ ∼ 880 μm) and with high angular resolution (∼ 2″-3″). We find that the large-scale global direction of the field, which is perpendicular to the observed polarization, appears to be along the dust ridge where the emission peaks. On smaller scales we find that the field structure is significantly different for the two components of the binary. The first component, source A, shows a magnetic field structure that is "hourglass" shaped as predicted from theoretical models of low-mass star formation in the presence of strong magnetic fields. However, the other component, source B, shows a relatively ordered magnetic field with no evidence of any deformation. We have possibly detected a third younger outflow from source A as seen in the SiO emission, which is in addition to the two well-known powerful bipolar outflows in this kinematically active region. There is an observed decrease in polarization toward the center and this "polarization hole" is similar to decreases seen in other young star-forming regions. Our calculations show that in IRAS 16293 the magnetic energy is stronger than the turbulent energy but is approximately similar to the centrifugal energy. There is a considerable misalignment between the outflow direction and the magnetic field axis, and this is roughly in agreement with model predictions where the magnetic energy is comparable to the centrifugal energy. In conjunction with other observations of the kinematics as determined from the outflow energetics and chemical differentiation, we find that our results provide additional evidence to show that the two protostars appear to be in different stages during their evolution. © 2009. The American Astronomical Society. All rights reserved.
• Yusef-Zadeh, F., Bushouse, H., Wardle, M., Heinke, C., Roberts, D. A., Dowell, C. D., Brunthaler, A., Reid, M. J., Martin, C. L., Marrone, D. P., Porquet, D., Grosso, N., Dodds-Eden, K., Bower, G. C., Wiesemeyer, H., Miyazaki, A., Pal, S., Gillessen, S., Goldwurm, A., , Trap, G., et al. (2009). Simultaneous multi-wavelength observations of sgr A* during 2007 april 1-11. Astrophysical Journal Letters, 706(1), 348-375.
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  Abstract: We report the detection of variable emission from Sgr A* in almost all wavelength bands (i.e., centimeter, millimeter, submillimeter, near-IR, and X-rays) during a multi-wavelength observing campaign. Three new moderate flares are detected simultaneously in both near-IR and X-ray bands. The ratio of X-ray to near-IR flux in the flares is consistent with inverse Compton scattering of near-IR photons by submillimeter emitting relativistic particles which follow scaling relations obtained from size measurements of Sgr A*. We also find that the flare statistics in near-IR wavelengths is consistent with the probability of flare emission being inversely proportional to the flux. At millimeter wavelengths, the presence of flare emission at 43 GHz (7 mm) using the Very Long Baseline Array with milliarcsecond spatial resolution indicates the first direct evidence that hourly timescale flares are localized within the inner 30 × 70 Schwarzschild radii of Sgr A*. We also show several cross-correlation plots between near-IR, millimeter, and submillimeter light curves that collectively demonstrate the presence of time delays between the peaks of emission up to 5 hr. The evidence for time delays at millimeter and submillimeter wavelengths are consistent with the source of emission initially being optically thick followed by a transition to an optically thin regime. In particular, there is an intriguing correlation between the optically thin near-IR and X-ray flare and optically thick radio flare at 43 GHz that occurred on 2007 April 4. This would be the first evidence of a radio flare emission at 43 GHz delayed with respect to the near-IR and X-ray flare emission. The time delay measurements support the expansion of hot self-absorbed synchrotron plasma blob and weaken the hot spot model of flare emission. In addition, a simultaneous fit to 43 and 84 GHz light curves, using an adiabatic expansion model of hot plasma, appears to support a power law rather than a relativistic Maxwellian distribution of particles. © 2009. The American Astronomical Society. All rights reserved.
• Bonamente, M., Joy, M., LaRoque, S. J., Carlstrom, J. E., Nagai, D., & Marrone, D. P. (2008). Scaling relations from sunyaev-zel'dovich effect and Chandra X-ray measurements of high-redshift galaxy clusters. Astrophysical Journal, 675(1), 106-114.
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  Abstract: We present Sunyaev-Zel'dovich Effect (SZE) scaling relations for 38 massive galaxy clusters at redshifts 0.14 ≤ z ≤ 0.89, observed with both the Chandra X-ray Observatory and the centimeter-wave SZE imaging system at the BIMA and OVRO interferometric arrays. An isothermal β-model with the central 100 kpc excluded from the X-ray data is used to model the intracluster medium and to measure global cluster properties. For each cluster, we measure the X-ray spectroscopic temperature, SZE gas mass, total mass, and integrated Compton y-parameters within r2500. Our measurements are in agreement with the expectations based on a simple self-similar model of cluster formation and evolution. We compare the cluster properties derived from our SZE observations with and without Chandra spatial and spectral information and find them to be in good agreement. We compare our results with cosmological numerical simulations and find that simulations that include radiative cooling, star formation, and feedback match well both the slope and normalization of our SZE scaling relations. © 2008. The American Astronomical Society. All rights reserved.
• Girart, J. M., Rao, R., & Marrone, D. P. (2008). SMA observations of the magnetic fields around a low-mass protostellar system. Astrophysics and Space Science, 313(1-3), 87-90.
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  Abstract: Observations of the submillimeter polarized dust emission is an important tool to study the role of the magnetic fields in the evolutions of molecular clouds and in the star formation processes. The Submillimeter Array (SMA) is the first imaging submillimeter interferometer. The installation of quarter wave plates in front of the 345 GHz receivers has allowed to carry out polarimetric observations. We present high angular resolution 345 GHz SMA observations of polarized dust emission towards the low-mass protostellar system NGC 1333 IRAS 4A. We show that in this system the observed magnetic field morphology is in agreement with the standard theoretical models of formation of low-mass stars in magnetized molecular clouds at scales of a few hundred AU; gravity has overcome magnetic support and the magnetic field traces a clear hourglass shape. The magnetic field is substantially more important than turbulence in the evolution of the system and the initial misalignment of the magnetic and spin axes may have been important in the formation of the binary system. © 2007 Springer Science+Business Media B.V.
• Marrone, D. P., & Rao, R. (2008). The submillimeter array polarimeter. Proceedings of SPIE - The International Society for Optical Engineering, 7020.
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  Abstract: We describe the Submillimeter Array (SMA) Polarimeter, a polarization converter and feed multiplexer installed on the SMA. The Polarimeter uses narrow-band quarter-wave plates to generate circular polarization sensitivity from the linearly-polarized SMA feeds. The wave plates are mounted in rotation stages under computer control so that the polarization handedness of each antenna is rapidly selectable. Positioning of the wave plates is found to be highly repeatable, better than 0.2 degrees. Although only a single polarization is detected at any time, all four cross correlations of left- and right-circular polarization are efficiently sampled on each baseline through coordinated switching of the antenna polarizations in Walsh function patterns. The initial set of anti-reflection coated quartz and sapphire wave plates allows polarimetry near 345 GHz; these plates have been have been used in observations between 325 and 350 GHz. The frequency-dependent cross-polarization of each antenna, largely due to the variation with frequency of the retardation phase of the single-element wave plates, can be measured precisely through observations of bright point sources. Such measurements indicate that the cross-polarization of each antenna is a few percent or smaller and stable, consistent with the expected frequency dependence and very small alignment errors. The Polarimeter is now available for general use as a facility instrument of the SMA.
• Marrone, D. P., Baganoff, F. K., Morris, M. R., Moran, J. M., Ghez, A. M., Hornstein, S. D., Dowell, C. D., Muñoz, D., Bautz, M. W., Ricker, G. R., Brandt, W. N., Garmire, G. P., Lu, J. R., Matthews, K., Zhao, J. -., Rao, R., & Bower, G. C. (2008). An x-ray, infrared, and submillimeter flare of Sagittarius A*. Astrophysical Journal, 682(1), 373-383.
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  Abstract: Energetic flares are observed in the Galactic supermassive black hole Sagittarius A* fromradio to X-ray wavelengths. On a few occasions, simultaneous flares have been detected in IR and X-ray observations, but clear counterparts at longer wavelengths have not been seen. We present a flare observed over several hours on 2006 July 17 with the Chandra X-Ray Observatory, the Keck II telescope, the Caltech Submillimeter Observatory, and the Submillimeter Array. All telescopes observed strong flare events, but the submillimeter peak is found to occur nearly 100 minutes after the X-ray peak. Submillimeter polarization data show linear polarization in the excess flare emission, increasing from 9% to 17% as the flare passes through its peak, consistent with a transition from optically thick to thin synchrotron emission. The temporal and spectral behavior of the flare require that the energetic electrons responsible for the emission cool faster than expected from their radiative output. This is consistent with adiabatic cooling in an expanding emission region, with X-rays produced through self-Compton scattering, although not consistent with the simplest model of such expansion. We also present a submillimeter flare that followed a bright IR flare on 2005 July 31. Compared to 2006, this event had a larger peak IR flux and similar submillimeter flux, but it lacked measurable X-ray emission. It also showed a shorter delay between the IR and submillimeter peaks. Based on these events we propose a synchrotron and self-Compton model to relate the submillimeter lag and the variable IR/X-ray luminosity ratio. © 2008. The American Astronomical Society. All rights reserved.
• Matthews, B., Bergin, E., Crapsi, A., Hogerheijde, M., Jørgensen, J., Marrone, D., & Rao, R. (2008). The Class 0 source Barnard 1c : MMMost recent results. Astrophysics and Space Science, 313(1-3), 65-68.
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  Abstract: We present our most recent results from an ongoing study of the Class 0 source Barnard 1c in Perseus. This source is of particular interest because it exhibits evidence of strong alignment of grains all the way to the core's centre, which is contrary to all other low-mass protostellar cores observed to date. Our goal is to clarify the source of poor alignment in other sources by identifying the source of strong alignment in B1c. A central cavity has been identified in N2H+ emission; its anticorrelation with C18O emission suggests that heating in the centre has released CO from grain mantles, in turn destroying N2H+. We present sensitivity-limited, high spatial resolution polarimetry data from the SubMillimeter Array and discuss the potential implications of these data. © 2007 Springer Science+Business Media B.V.
• Minier, V., Olmi, L., Lagage, P. -., Spinoglio, L., Durand, G. A., Daddi, E., Galilei, D., Gallée, H., Kramer, C., Marrone, D., Pantin, E., Sabbatini, L., Schneider, N., Tothill, N. F., Valenziano, L., & Veyssière, C. (2008). SUBMM/FIR astronomy in Antarctica: Potential for a large telescope facility. EAS Publications Series, 33, 21-40.
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  Abstract: Preliminary site testing datasets suggest that Dome C in Antarctica is one of the best sites on Earth for astronomical observations in the 200 to 500-μm regime, i.e. for far-infrared (FIR) and submillimetre (submm) astronomy. We present an overview of potential science cases that could be addressed with a large telescope facility at Dome C. This paper also includes a presentation of the current knowledge about the site characterics in terms of atmospheric transmission, stability, sky noise and polar constraints on telescopes. Current and future site testing campaigns are finally described. © EAS, EDP Sciences 2008.
• Mochejska, B. J., Stanek, K. Z., Sasselov, D. D., Szentgyorgyi, A. H., Cooper, R. L., Hickox, R. C., Hradecky, V., Marrone, D. P., Winn, J. N., & Schwarzenberg-Czerny, A. (2008). Planets in stellar clusters extensive search. V. Search for planets and identification of 18 new variable stars in the old open cluster NGC 188. Acta Astronomica, 58(3), 263-278.
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  Abstract: We have undertaken a long-term project, Planets in Stellar Clusters Extensive Search (PISCES), to search for transiting planets in open clusters. In this paper we present the results for NGC 188, an old, rather populous cluster. We have monitored the cluster for more than 87 hours, spread over 45 nights. We have not detected any good transiting planet candidates. We have discovered 18 new variable stars in the cluster, bringing the total number of identified variables to 28, and present for them high precision light curves, spanning 15 months.
• Moran, J. M., Marrone, D. P., Zhao, J. -., & Rao, R. (2008). The polarization properties of sgr A* at submillimeter wavelengths. ESO Astrophysics Symposia, 2008, 163-169.
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  Abstract: We have placed an upper limit on the magnitude of the rotation measure of 7 × 105 rad m-2 for the putative Faraday screen (magnetized plasma) in front of Sgr A*, the radio source associated with the black hole in the Galactic Center. There is evidence that the actual rotation measure is about -5 × 105 rad m-2. With a simple model of equipartition of energy and reasonable inner radius for the screen, the accretion rate is estimated to be less than 10-6 M⊙ yr -1. In addition, we have detected, for the first time, intra-day variability in the polarization of Sgr A*, which may be due to either intrinsic variations in Sgr A* or variations in the composition of the Faraday screen. © 2008 Springer-Verlag Berlin Heidelberg.
• Qin, S., Zhao, J., Moran, J. M., Marrone, D. P., Patel, N. A., Wang, J., Liu, S., & Kuan, Y. (2008). Infall and outflow of molecular gas in Sgr B2. Astrophysical Journal, 677(1), 353-372.
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  Abstract: Observations of two H2CO (303-202 and 321-220) lines and continuum emission at 1.3 mm toward Sgr B2(N) and Sgr B2(M) have been carried out with the SMA. The mosaic maps of Sgr B2(N) and Sgr B2(M) in both continuum and lines show a complex distribution of dust and molecular gas in both clumps and filaments surrounding the compact star formation cores. We have observed a decelerating outflow originated from the Sgr B2( M ) core, showing that both the redshifted and blueshifted outflow components have a common terminal velocity. This terminal velocity is 58 ±2 km s-1. It provides an excellent method for determination of the systematic velocity of the molecular cloud. The SMA observations have also shown that a large fraction of absorption against the two continuum cores is redshifted with respect to the systematic velocities of Sgr B2(N ) and Sgr B2(M ), respectively, suggesting that the majority of the dense molecular gas is flowing into the two major cores where massive stars have been formed. We have solved the radiative transfer in a multilevel system with LVG approximation. The observed H2CO line intensities and their ratios can be adequately fitted with this model for the most of the gas components. However, the line intensities between the higher energy level transition H2CO(3 21-220) and the lower energy level transition H 2CO(321-220) is reversed in the redshifted outflow region of Sgr B2(M), suggesting the presence of inversion in population between the ground levels in the two K ladders (K -1= 0 and 2). The possibility of weak maser processes for the H2CO emission in Sgr B2(M) is discussed. © 2008. The American Astronomical Society. All rights reserved.
• Coble, K., Bonamente, M., Carlstrom, J. E., Dawson, K., Hasler, N., Holzapfel, W., Joy, M., LaRoque, S., Marrone, D. P., & Reese, E. D. (2007). Radio sources toward galaxy clusters at 30 GHz. Astronomical Journal, 134(3), 897-905.
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  Abstract: Extragalactic radio sources are a significant contaminant in cosmic microwave background and Sunyaev-Zel'dovich effect experiments. Deep interferometric observations with the BIMA and OVRO arrays are used to characterize the spatial, spectral, and flux distributions of radio sources toward massive galaxy clusters at 28.5 GHz. We compute counts of millijansky source fluxes from 89 fields centered on known massive galaxy clusters and 8 noncluster fields. We find that source counts in the inner regions of the cluster fields (within 0,5′ of the cluster center) are a factor of 8.9-2.8+4.3 times higher than counts in the outer regions of the cluster fields (radius greater than 0.5′). Counts in the outer regions of the cluster fields are, in turn, a factor of 3.3-1.8+4.1 greater than those in the noncluster fields. Counts in the noncluster fields are consistent with extrapolations from the results of other surveys. We compute the spectral indices of millijansky sources in the cluster fields between 1.4 and 28.5 GHz and find a mean spectral index of α = 0.66 with an rms dispersion of 0.36, where flux S ∝ V-α. The distribution is skewed, with a median spectral index of 0.72 and 25th and 75th percentiles of 0.51 and 0.92, respectively. This is steeper than the spectral indices of stronger field sources measured by other surveys. © 2007, The American Astronomical Society. All rights reserved.
• Macías-Pérez, J., Lagache, G., Maffei, B., Ganga, K., Bourrachot, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Aumont, J., Bargot, S., Bartlett, J., Benoît, A., Bernard, J., Bhatia, R., Blanchard, A., Bock, J. J., Boscaleri, A., Bouchet, F. R., , Camus, P., et al. (2007). Archeops in-flight performance, data processing, and map making. Astronomy and Astrophysics, 467(3), 1313-1344.
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  Abstract: Aims. Archeops is a balloon-borne experiment inspired by the Planck satellite and its high frequency instrument (HFI). It is designed to measure the cosmic microwave background (CMB) temperature anisotropies at high angular resolution (∼12 arcmin) over a large fraction of the sky (around 30%) at 143, 217, 353, and 545 GHz. The Archeops 353 GHz channel consists of three pairs of polarized sensitive bolometers designed to detect the polarized diffuse emission of Galactic dust. Methods. In this paper we present an update of the instrumental setup, as well as the flight performance for the last Archeops flight campaign (February 2002 from Kiruna, Sweden). We also describe the processing and analysis of the Archeops time-ordered data for that campaign, which led to measurement of the CMB anisotropy power spectrum in the multipole range ℓ = 10-700 and to the first measurements of both the polarized emission of dust at large angular scales and its power spectra in the multipole range ℓ = 3-70 Results. We present maps covering approximately 30% of the sky. These maps contain Galactic emission, including the Galactic plane, in the four Archeops channels at 143, 217, 353, and 545 GHz and CMB anisotropies at 143 and 217 GHz. These are one of the first sub-degree-resolution maps in the millimeter and submillimeter ranges of the large angular-scale diffuse Galactic dust emission and CMB temperature anisotropies, respectively. © ESO 2007.
• Marrone, D. P., Moran, J. M., Zhao, J., & Rao, R. (2007). An unambiguous detection of faraday rotation in sagittarius A*. Astrophysical Journal, 654(1 II), L57-L60.
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  Abstract: The millimeter/submillimeter wavelength polarization of Sgr A* is known to be variable in both magnitude and position angle on timescales down to a few hours. The unstable polarization has prevented measurements made at different frequencies and different epochs from yielding convincing measurements of Faraday rotation in this source. Here we present observations made with the Submillimeter Array polarimeter at 227 and 343 GHz with sufficient sensitivity to determine the rotation measure at each band without comparing position angles measured at separate epochs. We find the 10-epoch mean rotation measure to be (-5.6 ± 0.7) × 105 rad m-2; the measurements are consistent with a constant value. We conservatively assign a 3 σ upper limit of 2 × 105 rad m-2 to rotation measure changes, which limits accretion rate fluctuations to 25%. This rotation measure detection limits the accretion rate to less than 2 × 10-7 M⊙ yr-1 if the magnetic field is near equipartition, ordered, and largely radial, while a lower limit of 2 × 10-9 M⊙ yr-1 holds even for a subequipartition, disordered, or toroidal field. The mean intrinsic position angle is 167° ± 7° and we detect variations of 31-9+18 deg. These variations must originate in the submillimeter photosphere, rather than arising from rotation measure changes. © 2007. The American Astronomical Society. All rights reserved.
• Eckart, A., Baganoff, F. K., Schödel, R., Morris, M., Genzel, R., Bower, G. C., Marrone, D., Moran, J. M., Viehmann, T., Bautz, M. W., Brandt, W. N., Garmire, G. P., Ott, T., Trippe, S., Ricker, G. R., Straubmeier, C., Roberts, D. A., Yusef-Zadeh, F., Zhao, J. H., & Rao, R. (2006). The flare activity of Sagittarius A* New coordinated mm to X-ray observations. Astronomy and Astrophysics, 450(2), 535-555.
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  Abstract: Context. We report new simultaneous near-infrared/sub-millimeter/X-ray observations of the Sgr A* counterpart associated with the massive 3-4 × 106 M⊙ black hole at the Galactic Center. Aims. We investigate the physical processes responsible for the variable emission from Sgr A*. Methods. The observations have been carried out using the NACO adaptive optics (AO) instrument at the European Southern Observatory's Very Large Telescope* and the ACIS-I instrument aboard the Chandra X-ray Observatory as well as the Submillimeter Array SMA** on Mauna Kea, Hawaii, and the Very Large Array*** in New Mexico. Results. We detected one moderately bright flare event in the X-ray domain and 5 events at infrared wavelengths. The X-ray flare had an excess 2-8 keV luminosity of about 33 × 1033 erg/s. The duration of this flare was completely covered in the infrared and it was detected as a simultaneous NIR event with a time lag of ≤10 min. Simultaneous infrared/X-ray observations are available for 4 flares. All simultaneously covered flares, combined with the flare covered in 2003, indicate that the time-lag between the NIR and X-ray flare emission is very small and in agreement with a synchronous evolution. There are no simultaneous flare detections between the NIR/X-ray data and the VLA and SMA data. The excess flux densities detected in the radio and sub-millimeter domain may be linked with the flare activity observed at shorter wavelengths. Conclusions. We find that the flaring state can be explained with a synchrotron self-Compton (SSC) model involving up-scattered submillimeter photons from a compact source component. This model allows for NIR flux density contributions from both the synchrotron and SSC mechanisms. Indications for an exponential cutoff of the NIR/MIR synchrotron spectrum allow for a straightforward explanation of the variable and red spectral indices of NIR flares. © ESO 2006.
• Girart, J. M., Rao, R., & Marrone, D. P. (2006). Magnetic fields in the formation of sun-like stars. Science, 313(5788), 812-814.
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  PMID: 16902132;Abstract: We report high-angular-resolution measurements of polarized dust emission toward the low-mass protostellar system MGC 1333 IRAS 4A. We show that in this system the observed magnetic field morphology is in agreement with the standard theoretical models of the formation of Sun-like stars in magnetized molecular clouds at scales of a few hundred astronomical units; gravity has overcome magnetic support, and the magnetic field traces a clear hourglass shape. The magnetic field is substantially more important than turbulence in the evolution of the system, and the initial misalignment of the magnetic and spin axes may have been important in the formation of the binary system.
• Marrone, D. P., Moran, J. M., Zhao, J., & Rao, R. (2006). Interferometric measurements of variable 340 GHz linear polarization in sagittarius A*. Astrophysical Journal Letters, 640(1 I), 308-318.
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  Abstract: Using the Submillimeter Array, we have made the first high angular resolution measurements of the linear polarization of Sagittarius A* at submillimeter wavelengths and the first detection of intraday variability in its linear polarization. We detected linear polarization at 340 GHz (880 μm) at several epochs. At the typical resolution of 1″.4 × 2″.2, the expected contamination from the surrounding (partially polarized) dust emission is negligible. We found that both the polarization fraction and the position angle are variable, with the polarization fraction dropping from 8.5% to 2.3% over 3 days. This is the first significant measurement of variability in the linear polarization fraction in this source. We also found variability in the polarization and total intensity within single nights, although the relationship between the two is not clear from these data. The simultaneous 332 and 342 GHz position angles are the same, setting a 1 σ rotation measure (RM) upper limit of 7 × 105 rad m-2. From position angle variations and comparison of "quiescent" position angles observed here and at 230 GHz, we infer that the RM is a few times 105 rad m -2, a factor of a few below our direct detection limit. A generalized model of the RM produced in the accretion flow suggests that the accretion rate at small radii must be low, below 10-6-10-7 M ⊙ yr-1 depending on the radial density and temperature profiles, but in all cases below the gas capture rate inferred from X-ray observations. © 2006 The American Astronomical Society. All rights reserved.
• Marrone, D. P., Moran, J. M., Zhao, J., & Rao, R. (2006). The submillimeter polarization of Sgr A*. Journal of Physics: Conference Series, 54(1), 354-362.
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  Abstract: We report on the submillimeter properties of Sgr A* derived from observations with the Submillimeter Array and its polarimeter. We ftid that the spectrum of Sgr A* between 230 and 690 GHz is slightly decreasing when measured simultaneously, indicating a transition to optically thin emission around 300-400 GHz. We also present very sensitive and well calibrated measurements of the polarization of Sgr A* at 230 and 345 GHz. With these data we are able to show for the frst time that the polarization of Sgr A* varies on hour timescales, as has been observed for the total intensity. On one night we fhd variability that may arise from a polarized "blob" orbiting the black hole. Finally, we use the ensemble of observations to determine the rotation measure. This represents the frst statistically significant rotation measure determination and the only one made without resorting to comparing position angles measured at separate epochs. We frid a rotation measure of (-5.6 0.7) × 105 rad m2, with no evidence for variability on inter-day timescales at the level of the measurement error. The stability constrains interday flictuations in the accretion rate to 8%. The mean intrinsic polarization position angle is 167°7° and we detect variations of 31+18-9 degrees. This separation of intrinsic polarization changes and possible rotation measure flictuations is now possible because of the frequency coverage and sensitivity of our data. The observable rotation measure restricts the accretion rate to the range 2 × 10-7 M yr-1 to 2 × 10-9 M yr-1, if the magnetic ffeld is near equipartition and ordered. © 2006 IOP Publishing Ltd.
• Qin, S., Zhao, J., Moran, J. M., Marrone, D., Patel, N., Liu, S., Kuan, Y., & Wang, J. (2006). Infall, fragmentation, and outflow in Sgr B2. Journal of Physics: Conference Series, 54(1), 468-473.
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  Abstract: Observations of H2CO lines and continuum at 1.3 mm towards Sgr B2(N) and Sgr B2(M) cores were carried out with the SMA. We imaged H 2CO line absorption against the continuum cores and the surrounding line emission clumps. The results show that the majority of the dense gas is falling into the major cores where massive stars have been formed. The filaments and clumps of the continuum and gas are detected outside of Sgr B2(N) and Sgr B2(M) cores. Both the spectra and moment analysis show the presence of outflows from Sgr B2(M) core. The H2CO gas in the red-shifted outflow of Sgr B2(M) appears to be excited by a non-LTE process which might be related to the shocks in the outflow. © 2006 IOP Publishing Ltd.
• Tong, C. E., Kawamura, J., Marrone, D., Loudkov, D., Paine, S., Blundell, R., Barrientos, C., & Lühr, D. (2006). A 1.5 THz hot electron bolometer receiver for ground-based Terahertz astronomy in Northern Chile. Proceedings of SPIE - The International Society for Optical Engineering, 6373.
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  Abstract: A 1.5 THz superconducting receiver has been in operation at the Receiver Lab Telescope of the Smithsonian Astrophysical Observatory in Northern Chile since December 2004. This receiver incorporates a Hot Electron Bolometer (HEB) mixer chip made from a thin film of Niobium Titanium Nitride (NbTiN), which is mounted in a precision-machined waveguide mixer block attached to a corrugated waveguide horn assembly. With a noise temperature of around 1500 K, this receiver is sensitive enough for use in the pioneering field of ground-based terahertz spectral-line astronomy. A number of innovative techniques have been employed in the construction and deployment of this receiver. These include near-field vector beam mapping to enable accurate coupling to the telescope optics, the use of tunerless planar-diode based local oscillator unit capable of generating a few μW at 1.5 THz, and special calibration techniques required for terahertz astronomy. In this paper, we will report on the design, set-up and operation of this state-of-the-art instrument.
• Mochejska, B. J., Stanek, K. Z., Sasselov, D. D., Szentgyorgyi, A. H., Bakos, G., Devor, J., Hradecky, V., Marrone, D. P., Winn, J. N., & Zaldarriaga, M. (2005). Planets in stellar clusters extensive search. III. A search for transiting planets in the metal-rich open cluster NGC 6791. Astronomical Journal, 129(6), 2856-2868.
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  Abstract: We have undertaken a long-term project, Planets in Stellar Clusters Extensive Search (PISCES), to search for transiting planets in open clusters. In this paper we present the results for NGC 6791, a very old, populous, metal-rich cluster. We have monitored the cluster for over 300 hr, spread over 84 nights. We have not detected any good transiting planet candidates. Given the photometric precision and temporal coverage of our observations and the current best estimates for the frequency and radii of short-period planets, the expected number of detectable transiting planets in our sample is 1.5. We have discovered 14 new variable stars in the cluster, most of which are eclipsing binaries, and present high-precision light curves spanning 2 years for these new variables and also the previously known variables. © 2005. The American Astronomical Society. All rights reserved.
• Benoît, A., Ade, P., Amblard, A., Ansari, R., Aubourg, É., Bargot, S., Bartlett, J. G., Bernard, J., Bhatia, R. S., Blanchard, A., Bock, J. J., Boscaleri, A., Bouchet, F. R., Bourrachot, A., Camus, P., Couchot, F., Bernardis, P. D., Delabrouille, J., Désert, F., , Doré, O., et al. (2004). First detection of polarization of the submillimetre diffuse galactic dust emission by Archeops. Astronomy and Astrophysics, 424(2), 571-582.
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  Abstract: We present the first determination of the Galactic polarized emission at 353 GHz by Archeops. The data were taken during the Arctic night of February 7, 2002 after the balloon-borne instrument was launched by CNES from the Swedish Esrange base near Kiruna. In addition to the 143 GHz and 217 GHz frequency bands dedicated to CMB studies, Archeops had one 545 GHz and six 353 GHz bolometers mounted in three polarization-sensitive pairs that were used for Galactic foreground studies. We present maps of the I, Q, U Stokes parameters over 17% of the sky and with a 13 arcmin resolution at 353 GHz (850 μm). They show a significant Galactic large scale polarized emission coherent on the longitude ranges [100, 120] and [180, 200] deg. with a degree of polarization at the level of 4-5%, in agreement with expectations from starlight polarization measurements. Some regions in the Galactic plane (Gem OB1, Cassiopeia) show an even stronger degree of polarization in the range 10-20%. These findings provide strong evidence for a powerful grain alignment mechanism throughout the interstellar medium and a coherent magnetic field coplanar to the Galactic plane. This magnetic field pervades even some dense clouds. Extrapolated to high Galactic latitude, these results indicate that interstellar dust polarized emission is the major foreground for PLANCK-HFI CMB polarization measurements.
• Beuther, H., Zhang, Q., Greenhill, L. J., Reid, M. J., Wilner, D., Keto, E., Marrone, D., Ho, P. T., Moran, J. M., Rao, R., Shinnaga, H., & Liu, S. -. (2004). Subarcsecond submillimeter continuum observations of orion KL. Astrophysical Journal Letters, 616(1 II), L31-L34.
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  Abstract: We present the first 865 μm continuum image with subarcsecond resolution obtained with the Submillimeter Array. These data resolve the Orion KL region into the hot core, the nearby radio source I, the submillimeter counterpart to the infrared source n (radio source L), and new submillimeter continuum sources. The radio to submillimeter emission from source I can be modeled as either the result of proton-electron free-free emission that is optically thick to ∼100 GHz plus dust emission that accounts for the majority of the submillimeter flux, or H free-free emission that gives rise to a power-law spectrum with a power-law index of ∼1.6. The latter model would indicate similar physical conditions as found in the inner circumstellar environment of Mira variable stars. Future subarcsecond resolution observations at shorter submillimeter wavelengths should easily discriminate between these two possibilities. The submillimeter continuum emission toward source n can be interpreted in the framework of emission from an accretion disk.
• Marrone, D. P., Battat, J., Bensch, F., Blundell, R., Diaz, M., Gibson, H., Hunter, T., Meledin, D., Paine, S., Papa, D. C., Radford, S., Smith, M., & Tong, E. (2004). A map of OMC-1 in CO J = 9→8. Astrophysical Journal Letters, 612(2 I), 940-945.
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  Abstract: The distribution of 12C16O J = 9 → 8 (1.037 THz) emission has been mapped in OMC-1 at 35 points with. 84″ resolution. This is the first map of this source in this transition and only the second velocity-resolved ground-based observation of a line in the THz frequency band. There is emission present at all points in the map, a region roughly 4′×6′ in size, with peak antenna temperature dropping only near the edges. Away from the Orion KL outflow, the velocity structure suggests that most of the emission comes from the OMC-1 photon-dominated region, with a typical line width of 3-6 km s-1. Large velocity gradient modeling of the emission in J = 9 → 8 and six lower transitions suggests that the lines originate in regions with temperatures around 120 K and densities of at least 103.5 cm-3 near θ1 C Ori and at the Orion bar, and from 70 K gas at around 104 cm-3 southeast and west of the bar. These observations are among the first made with the 0.8 m Smithsonian Astrophysical Observatory Receiver Lab Telescope, a new instrument designed to observe at frequencies above 1 THz from an extremely high and dry site in northern Chile.
• Benoît, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Bargot, S., Bartlett, J. G., Bernard, J., Bhatia, R. S., Blanchard, A., Bock, J. J., Boscaleri, A., Bouchet, F. R., Bourrachot, A., Camus, P., Couchot, F., Bernardis, P. D., Delabrouille, J., Désert, F., , Doré, O., et al. (2003). Cosmological constraints from archeops. Astronomy and Astrophysics, 399(3), L25-L30.
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  Abstract: We analyze the cosmological constraints that Archeops (Benoît et al. 2003) places on adiabatic cold dark matter models with passive power-law initial fluctuations. Because its angular power spectrum has small bins in ℓ and large ℓ coverage down to COBE scales, Archeops provides a precise determination of the first acoustic peak in terms of position at multipole lpeak = 220 ± 6, height and width. An analysis of Archeops data in combination with other CMB datasets constraints the baryon content of the Universe, Ωbh2 = 0.022-0.004+0.003, compatible with Big-Bang nucleosynthesis and with a similar accuracy. Using cosmological priors obtained from recent non-CMB data leads to yet tighter constraints on the total density, e.g. Ωtot = 1.00-0.02+0.03 using the HST determination of the Hubble constant. An excellent absolute calibration consistency is found between Archeops and other CMB experiments, as well as with the previously quoted best fit model. The spectral index n is measured to be 1.04-0.12+0.10 when the optical depth to reionization, τ, is allowed to vary as a free parameter, and 0.96-0.04+0.03 when τ is fixed to zero, both in good agreement with inflation.
• Benoît, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Bargot, S., Bartlett, J. G., Bernard, J., Bhatia, R. S., Blanchard, A., Bock, J. J., Boscaleri, A., Bouchet, F. R., Bourrachot, A., Camus, P., Couchot, F., Bernardis, P. D., Delabrouille, J., Désert, F., , Doré, O., et al. (2003). The cosmic microwave background anisotropy power spectrum measured by archeops. Astronomy and Astrophysics, 399(3), L19-L23.
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  Abstract: We present a determination by the Archeops experiment of the angular power spectrum of the cosmic microwave background anisotropy in 16 bins over the multipole range ℓ = 15-350. Archeops was conceived as a precursor of the Planck HFI instrument by using the same optical design and the same technology for the detectors and their cooling. Archeops is a balloon-borne instrument consisting of a 1.5 m aperture diameter telescope and an array of 21 photometers maintained at ∼ 100 mK that are operating in 4 frequency bands centered at 143, 217, 353 and 545 GHz. The data were taken during the Arctic night of February 7, 2002 after the instrument was launched by CNES from Esrange base (Sweden). The entire data cover ∼30% of the sky. This first analysis was obtained with a small subset of the dataset using the most sensitive photometer in each CMB band (143 and 217 GHz) and 12.6% of the sky at galactic latitudes above 30 degrees where the foreground contamination is measured to be negligible. The large sky coverage and medium resolution (better than 15 arcmin) provide for the first time a high signal-to-noise ratio determination of the power spectrum over angular scales that include both the first acoustic peak and scales probed by COBE/DMR. With a binning of Δℓ = 7 to 25 the error bars are dominated by sample variance for ℓ below 200. A companion paper details the cosmological implications.
• Tong, C. E., Meledin, D. V., Marrone, D. P., Paine, S. N., Gibson, H., & Blundell, R. (2003). Near field vector beam measurements at 1 THz. IEEE Microwave and Wireless Components Letters, 13(6), 235-237.
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  Abstract: We have performed near-field vector beam measurements at 1.03 THz to characterize and align the receiver optics of a superconducting receiver. The signal source is a harmonic generator mounted on an X-Y translation stage. We model the measured two-dimensional complex beam pattern by a fundamental Gaussian mode, from which we derive the position of the beam center, the beam radius and the direction of propagation. By performing scans in the planes separated by 400 mm, we have confirmed that our beam pattern measurements are highly reliable.
• Benot, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Bartlett, J., Bernard, J. -., Bhatia, R. S., Blanchard, A., Bock, J. J., Boscaleri, A., Bouchet, F. R., Bourrachot, A., Camus, P., Couchot, F., Bernardis, P. D., Delabrouille, J., Désert, F., Doré, O., , Douspis, M., et al. (2002). Archeops: A high resolution, large sky coverage balloon experiment for mapping cosmic microwave background anisotropies. Astroparticle Physics, 17(2), 101-124.
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  Abstract: Archeops is a balloon-borne instrument dedicated to measuring cosmic microwave background (CMB) temperature anisotropies at high angular resolution (∼8′) over a large fraction (∼25%) of the sky in the millimetre domain. Based on Planck high frequency instrument technology, cooled bolometers (0.1 K) scan the sky in total power mode with large circles at constant elevation. During the course of a 24-h Arctic-night balloon flight, Archeops will observe a complete annulus on the sky in four frequency bands centered at 143, 217, 353 and 545 GHz with an expected sensitivity to CMB fluctuations of ∼100 μK for each of the 90 thousand 20′ average pixels. We describe the instrument and its performance obtained during a test flight from Trapani (Sicily) to Spain in July 1999. © 2002 Elsevier Science B.V. All rights reserved.
• Hanany, S., & Marrone, D. P. (2002). Comparison of designs of off-axis Gregorian telescopes for millimeter-wave large focal-plane arrays. Applied Optics, 41(22), 4666-4670.
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  PMID: 12153101;Abstract: We compare the diffraction-limited field of view (FOV) provided by four types of off-axis Gregorian telescopes: the classical Gregorian, the aplanatic Gregorian, and the designs that cancel astigmatism and both astigmatism and coma. The analysis is carried out with telescope parameters that are appropriate for satellite and balloonborne millimeter- and submillimeter-wave astrophysics. We find that the design that cancels both coma and astigmatism provides the largest flat FOV, ∼ 21 square deg. We also find that the FOV can be increased by ∼ 15% by means of optimizing the shape and location of the focal surface. © 2002 Optical Society of America.
• Narita, T., Grindlay, J. E., Jenkins, J. A., Perrin, M., Marrone, D., Murray, R., & Connell, B. (2002). Design and preliminary tests of a prototype CZT imaging array. Proceedings of SPIE - The International Society for Optical Engineering, 4497, 79-87.
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  Abstract: We report on the design and construction of a tiled Cadmium Zinc Telluride (CZT) detector array, suitable for use as an astronomical coded aperture imager. Four detector modules, each with 4 × 4 × 0.5 cm of CZT, readout by two 128 channel XA type ASICs, have been built and incorporated into a detector focal plane array. A passive shield/collimator surrounded by plastic scintillator encloses the detector on five sides and provides a 40 degree field of view. In this paper, we present our performance goals and some preliminary calibration results.

Proceedings Publications

• Blackburn, L., Doeleman, S., Dexter, J., G{\'omez}, J. L., Johnson, M. D., Palumbo, D. C., Weintroub, J., Bouman, K. L., Chael, A. A., Farah, J. R., Fish, V., Loinard, L., Lonsdale, C., Narayanan, G., Patel, N. A., Pesce, D. W., Raymond, A., Tilanus, R., Wielgus, M., , Akiyama, K., et al. (2019, sep). Studying Black Holes on Horizon Scales with VLBI Ground Arrays. In Astro2020: Decadal Survey on Astronomy and Astrophysics, APC white papers, 51.
• Johnson, M., Haworth, K., Pesce, D. W., Palumbo, D. C., Blackburn, L., Akiyama, K., Boroson, D., Bouman, K. L., Farah, J. R., Fish, V. L., Honma, M., Kawashima, T., Kino, M., Raymond, A., Silver, M., Weintroub, J., Wielgus, M., Doeleman, S. S., Kauffmann, J., , Keating, G. K., et al. (2019, sep). Studying black holes on horizon scales with space-VLBI. In Astro2020: Decadal Survey on Astronomy and Astrophysics, APC white papers, 51.
• Kim, J., & Marrone, D. (2018, sep). Tilted Beam Measurement of VLBI Receiver for the South Pole Telescope. In 29TH IEEE International Symposium on Space Terahertz Technology.
• Kim, J., Marrone, D., Beaudoin, C., Carlstrom, J., Doeleman, S., Folkers, T., Forbes, D., Greer, C., Lauria, E., Massingill, K., Mayer, E., Nguyen, C., Reiland, G., SooHoo, J., Stark, A., Vertatschitsch, L., Weintroub, J., & Young, A. (2018, jul). A VLBI receiving system for the South Pole Telescope. In SPIE Astronomical Telescopes + Instrumentation, 10708.
• Witzel, G., Becklin, E., Fazio, G., Smith, H., Morris, M., Baganoff, .., Willner, S., Hora, J., Martinez, G., Marrone, D., Herrero-Illana, R. .., & Ghez, A. (2018, jul). Recent results from observations of Sgr A* variability with the Spitzer & Chandra Space Telescopes. In 42nd COSPAR Scientific Assembly, 42.
• Johnson, M., Doeleman, S., Fish, V. L., Plambeck, R. L., Marrone, D. P., Kosowsky, M., Wardle, J. F., & Lu, R. (2014, jun). Polarimetry with the Event Horizon Telescope. In American Astronomical Society Meeting Abstracts, 224, #204.06.
• Keating, G. K., Bower, G. C., DeBoer, D. R., Heiles, C. E., & Marrone, D. P. (2014, jan). The Undiscovered CO: Charting the Molecular Gas of the Universe at High Redshift. In American Astronomical Society Meeting Abstracts, 223, #133.03.
• Kosowsky, M., Fish, V. L., Doeleman, S., Johnson, M., Lu, R., Marrone, D. P., Moran, J. M., Plambeck, R. L., Wardle, J. F., & Collaboration, E. (2014, jan). Moving Toward Polarimetry with the Event Horizon Telescope. In American Astronomical Society Meeting Abstracts, 223, #443.06.
• Bonamente, M., Carlstrom, J., Leitch, E., Joy, M., Marrone, D., Mantz, A., Muchovej, S., Plagge, T., & Reese, E. (2013, feb). Measurement of the cosmological distance scale using X-ray and Sunyaev-Zel'dovich effect observations of galaxy clusters. In IAU Symposium, 289, 339-343.
• Doeleman, S., Fish, V. L., Schenck, D., Beaudoin, C., Blundell, R., Bower, G. C., Broderick, A. E., Chamberlin, R., Freund, R., Friberg, P., Gurwell, M. A., Ho, P. T., Honma, M., Inoue, M., Krichbaum, T., Lamb, J. W., Loeb, A., Lonsdale, C. J., Marrone, D. P., , Moran, J. M., et al. (2013, jan). Jet-Launching Structure Resolved Near the Supermassive Black Hole in M87. In American Astronomical Society Meeting Abstracts, 221, #123.07.
• Fish, V. L., Doeleman, S., Marrone, D. P., Lu, R., Wardle, J. F., & Collaboration, E. (2013, jan). Polarimetric VLBI with the Event Horizon Telescope. In American Astronomical Society Meeting Abstracts, 221, #143.04.
• Hull, C., Plambeck, R. L., Bolatto, A. D., Bower, G. C., Carpenter, J. M., Crutcher, R., Fiege, J. D., Franzmann, E., Hakobian, N. S., Heiles, C. E., Houde, M., Hughes, A. M., Jameson, K., Kwon, W., Lamb, J. W., Looney, L., Marrone, D. P., Matthews, B. C., Mundy, L. G., , Pillai, T., et al. (2013, jan). The Distribution of Angles Between Outflows and Magnetic Fields in Low-mass Protostellar Cores. In American Astronomical Society Meeting Abstracts, 221, #426.04.
• Lu, R., Fish, V. L., Weintroub, J., Doeleman, S., Bower, G. C., Freund, R., Friberg, P., Ho, P. T., Honma, M., Inoue, M., Jorstad, S. G., Krichbaum, T., Marrone, D. P., Marscher, A. P., Moran, J. M., Oyama, T., Plambeck, R. L., Primiani, R., Shen, Z., , Tilanus, R., et al. (2013, jan). Fine Scale Structure of AGN Jets with 1.3 mm VLBI. In American Astronomical Society Meeting Abstracts, 221, #143.05.
• Marrone, D. P., & Team, S. S. (2013, jan). ALMA Observations of the Brightest Starbursts in the Universe. In American Astronomical Society Meeting Abstracts, 221, #221.02.
• Dawson, W., Wittman, D., Jee, J., Gee, P., Hughes, J. P., Marrone, D., Tyson, A., Schmidt, S., Muchovej, S., Thorman, P., Carlstrom, J., Bradac, M., Miyazaki, S., Mroczkowski, T., Lemaux, B., & Utsumi, Y. (2012, jan). Discovery of a Galaxy Cluster Merger in Unexplored Merger Phase-space. In American Astronomical Society Meeting Abstracts #219, 219, #223.07.
• Lindley, A., Landry, D., Bonamente, M., Joy, M., Bulbul, E., Carlstrom, J. E., Culverhouse, T. L., Gralla, M., Greer, C., Hawkins, D., Lamb, J. W., Leitch, E. M., Marrone, D. P., Miller, A., Mroczkowski, T., Muchovej, S., Plagge, T., & Woody, D. (2012, may). Calculating Cluster Masses via the Sunyaev-Zel'dovich Effect. In American Astronomical Society Meeting Abstracts #220, 220, #507.03.
• Miller, E. D., Bautz, M., Forman, W., Jones, C., Benson, B., Marrone, D., Reichardt, C., High, F. W., Brodwin, M., & Carlstrom, J. (2012, may). The Metal Abundance of High-Redshift Galaxy Clusters with Suzaku. In American Astronomical Society Meeting Abstracts #220, 220, #435.04.

Others

• Foley, R., Koekemoer, A., Spergel, D., Bianco, F., Capak, P., Dai, L., Dore, O., Fazio, G., Ferguson, H., Filippenko, A., Frye, B., Galbany, L., Gawiser, E., Gronwall, C., Hathi, N., Hirata, C., Hounsell, R., Jha, S., Kim, A., , Kelly, P., et al. (2018, nov). LSST Observing Strategy White Paper: LSST Observations of WFIRST Deep Fields. LSST Observing Strategy Whitepaper.