Publication Search Results

ID: 158983
Type: article
Authors: BICEP/Keck Collaboration; SPTpol Collaboration; Ade, P. A. R.; Ahmed, Z.; Amiri, M.; Anderson, A. J.; Austermann, J. E.; Avva, J. S.; Barkats, Denis; Thakur, R. Basu; Beall, J. A.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Bischoff, C. A.; Bleem, L. E.; Bock, J. J.; Boenish, H.; Bullock, E.; Buza, Victor; Carlstrom, J. E.; Chang, C. L.; Cheshire, J. R.; Chiang, H. C.; Chou, T. -L; Citron, R.; Connors, J.; Moran, C. Corbett; Cornelison, J.; Crawford, T. M.; Crites, A. T.; Crumrine, M.; Cukierman, A.; de Haan, T.; Dierickx, Marion; Dobbs, M. A.; Duband, L.; Everett, W.; Fatigoni, S.; Filippini, J. P.; Fliescher, S.; Gallicchio, J.; George, E. M.; St. Germaine, T.; Goeckner-Wald, N.; Goldfinger, D. C.; Grayson, J.; Gupta, N.; Hall, G.; Halpern, M.; Halverson, N. W.; Harrison, S.; Henderson, S.; Henning, J. W.; Hildebrandt, S. R.; Hilton, G. C.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Hui, H.; Irwin, K. D.; Kang, J.; Karkare, K. S.; Karpel, E.; Kefeli, S.; Kernasovskiy, S. A.; Knox, L.; Kovac, J. M.; Kuo, C. L.; Lau, K.; Lee, A. T.; Leitch, E. M.; Li, D.; Lowitz, A.; Manzotti, A.; McMahon, J. J.; Megerian, K. G.; Meyer, S. S.; Millea, M.; Mocanu, L. M.; Moncelsi, L.; Montgomery, J.; Nadolski, A.; Namikawa, T.; Natoli, T.; Netterfield, C. B.; Nguyen, H. T.; Nibarger, J. P.; Noble, G.; Novosad, V.; O'Brient, R.; Ogburn, R. W.; Omori, Y.; Padin, S.; Palladino, S.; Patil, S.; Prouve, T.; Pryke, C.; Racine, B.; Reichardt, C. L.; Reintsema, C. D.; Richter, S.; Ruhl, J. E.; Saliwanchik, B. R.; Schaffer, K. K.; Schillaci, A.; Schmitt, B. L.; Schwarz, R.; Sheehy, C. D.; Sievers, C.; Smecher, G.; Soliman, A.; Stark, Antony A.; Steinbach, B.; Sudiwala, R. V.; Teply, G. P.; Thompson, K. L.; Tolan, J. E.; Tucker, C.; Turner, A. D.; Umiltà, C.; Veach, T.; Vieira, J. D.; Vieregg, A. G.; Wandui, A.; Wang, G.; Weber, A. C.; Whitehorn, N.; Wiebe, D. V.; Willmert, J.; Wong, C. L.; Wu, W. L. K.; Yang, H.; Yefremenko, V.; Yoon, K. W.; Young, E.; Yu, C.; Zeng, L.; Zhang, C.; Bicep/Keck; Sptpol Collaborations
Abstract: We present a constraint on the tensor-to-scalar ratio, r , derived from measurements of cosmic microwave background (CMB) polarization B -modes with "delensing," whereby the uncertainty on r contributed by the sample variance of the gravitational lensing B -modes is reduced by cross-correlating against a lensing B -mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, BICEP/Keck, and Planck data. We expand the BICEP/Keck likelihood analysis framework to accept a lensing template and apply it to the BICEP/Keck dataset collected through 2014 using the same parametric foreground modeling as in the previous analysis. From simulations, we find that the uncertainty on r is reduced by ∼10 %, from σ (r )=0.024 to 0.022, which can be compared with a ∼26 % reduction obtained when using a perfect lensing template or if there were zero lensing B -modes. Applying the technique to the real data, the constraint on r is improved from r_0.050.05<0.082 (95% C.L.). This is the first demonstration of improvement in an r constraint through delensing.

ID: 159629
Type: article
Authors: Reichardt, C. L.; Patil, S.; Ade, P. A. R.; Anderson, A. J.; Austermann, J. E.; Avva, J. S.; Baxter, E.; Beall, J. A.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chaubal, P.; Chiang, H. C.; Chou, T. L.; Citron, R.; Moran, C. Corbett; Crawford, T. M.; Crites, A. T.; de Haan, T.; Dobbs, M. A.; Everett, W.; Gallicchio, J.; George, E. M.; Gilbert, A.; Gupta, N.; Halverson, N. W.; Harrington, N.; Henning, J. W.; Hilton, G. C.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; Knox, L.; Lee, A. T.; Li, D.; Lowitz, A.; Luong-Van, D.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Millea, M.; Mocanu, L. M.; Mohr, J. J.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Noble, G.; Novosad, V.; Omori, Y.; Padin, S.; Pryke, C.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Schaffer, K. K.; Shirokoff, E.; Sievers, C.; Smecher, G.; Spieler, H. G.; Staniszewski, Z.; Stark, Antony A.; Tucker, C.; Vanderlinde, K.; Veach, T.; Vieira, J. D.; Wang, G.; Whitehorn, N.; Williamson, R.; Wu, W. L. K.; Yefremenko, V.
Abstract: We report new measurements of millimeter-wave power spectra in the angular multipole range 2000 ≤ ℓ ≤ 11,000 (angular scales $5^{\prime} >rsim \theta >rsim 1^{\prime} $ ). By adding 95 and 150 GHz data from the low-noise 500 deg² SPTpol survey to the SPT-SZ three-frequency 2540 deg² survey, we substantially reduce the uncertainties in these bands. These power spectra include contributions from the primary cosmic microwave background, cosmic infrared background, radio galaxies, and thermal and kinematic Sunyaev-Zel'dovich (SZ) effects. The data favor a thermal SZ (tSZ) power at 143 GHz of ${D}_{3000}^{\mathrm{tSZ}}=3.42\pm 0.54\,\,\mu {{\rm{K}}}^{2}$ and a kinematic SZ (kSZ) power of ${D}_{3000}^{\mathrm{kSZ}}=3.0\pm 1.0\,\,\mu {{\rm{K}}}^{2}$ . This is the first measurement of kSZ power at ≥3σ. However, different assumptions about the CIB or SZ models can reduce the significance down to 2.4σ in the worst case. We study the implications of the measured kSZ power for the epoch of reionization under the Calabrese et al. model for the kSZ power spectrum and find the duration of reionization to be ${\rm{\Delta }}{z}_{\mathrm{re}}={1.1}_{-0.7}^{+1.6}$ ( ${\rm{\Delta }}{z}_{\mathrm{re}} survey, we substantially reduce the uncertainties in these bands. These power spectra include contributions from the primary cosmic microwave background, cosmic infrared background, radio galaxies, and thermal and kinematic Sunyaev-Zel'dovich (SZ) effects. The data favor a thermal SZ (tSZ) power at 143 GHz of ${D}_{3000}^{\mathrm{tSZ}}=3.42\pm 0.54\,\,\mu {{\rm{K}}}^{2}$ and a kinematic SZ (kSZ) power of ${D}_{3000}^{\mathrm{kSZ}}=3.0\pm 1.0\,\,\mu {{\rm{K}}}^{2}$ . This is the first measurement of kSZ power at ≥3σ. However, different assumptions about the CIB or SZ models can reduce the significance down to 2.4σ in the worst case. We study the implications of the measured kSZ power for the epoch of reionization under the Calabrese et al. model for the kSZ power spectrum and find the duration of reionization to be ${\rm{\Delta }}{z}_{\mathrm{re}}={1.1}_{-0.7}^{+1.6}$ ( ${\rm{\Delta }}{z}_{\mathrm{re}} survey, we substantially reduce the uncertainties in these bands. These power spectra include contributions from the primary cosmic microwave background, cosmic infrared background, radio galaxies, and thermal and kinematic Sunyaev-Zel'dovich (SZ) effects. The data favor a thermal SZ (tSZ) power at 143 GHz of ${D}_{3000}^{\mathrm{tSZ}}=3.42\pm 0.54\,\,\mu {{\rm{K}}}^{2}$ and a kinematic SZ (kSZ) power of ${D}_{3000}^{\mathrm{kSZ}}=3.0\pm 1.0\,\,\mu {{\rm{K}}}^{2}$ . This is the first measurement of kSZ power at ≥3σ. However, different assumptions about the CIB or SZ models can reduce the significance down to 2.4σ in the worst case. We study the implications of the measured kSZ power for the epoch of reionization under the Calabrese et al. model for the kSZ power spectrum and find the duration of reionization to be ${\rm{\Delta }}{z}_{\mathrm{re}}={1.1}_{-0.7}^{+1.6}$ ( ${\rm{\Delta }}{z}_{\mathrm{re}}²) and relaxes to ${\rm{\Delta }}{z}_{\mathrm{re}}< 5.2$ if the homogeneous kSZ power is decreased by the same amount.

ID: 159439
Type: article
Authors: Somboonpanyakul, Taweewat; McDonald, Michael A.; Gaspari, Massimo; Stalder, Brian; Stark, Antony A.
Abstract: We present optical follow-up observations for candidate clusters in the Clusters Hiding in Plain Sight survey, which is designed to find new galaxy clusters with extreme central galaxies that were misidentified as bright isolated sources in the ROSAT All-Sky Survey catalog. We identify 11 cluster candidates around X-ray, radio, and mid-IR-bright sources, including six well-known clusters, two false associations of foreground and background clusters, and three new candidates, which are observed further with Chandra. Of the three new candidates, we confirm two newly discovered galaxy clusters: CHIPS 1356-3421 and CHIPS 1911+4455. Both clusters are luminous enough to be detected in the ROSAT All-Sky Survey data if not because of their bright central cores. CHIPS 1911+4455 is similar in many ways to the Phoenix cluster, but with a highly disturbed X-ray morphology on large scales. We find the occurrence rate for clusters that would appear to be X-ray-bright point sources in the ROSAT All-Sky Survey (and any surveys with similar angular resolution) to be 2% ± 1%, and the occurrence rate of clusters with runaway cooling in their cores to be <1%, consistent with predictions of chaotic cold accretion. With the number of new groups and clusters predicted to be found with eROSITA, the population of clusters that appear to be point sources (due to a central QSO or a dense cool core) could be around 2000. Finally, this survey demonstrates that the Phoenix cluster is likely the strongest cool core at z < 0.7-anything more extreme would have been found in this survey.

ID: 159346
Type: article
Authors: Somboonpanyakul, Taweewat; McDonald, Michael; Bayliss, Matthew; Voit, Mark; Donahue, Megan; Gaspari, Massimo; Dahle, Håkon; Rivera-Thorsen, Emil; Stark, Antony
Abstract: We present high-resolution optical images from the Hubble Space Telescope, X-ray images from the Chandra X-ray Observatory, and optical spectra from the Nordic Optical Telescope for a newly discovered galaxy cluster, CHIPS1911+4455, at z = 0.485 ± 0.005. CHIPS1911+4455 was discovered in the Clusters Hiding in Plain Sight survey, which sought to discover galaxy clusters with extreme central galaxies that were misidentified as isolated X-ray point sources in the ROSAT All-Sky Survey. With new Chandra X-ray observations, we find the core (r = 10 kpc) entropy to be ${17}_{-9}^{+2}\,\mathrm{keV}\,{\mathrm{cm}}^{2}$ , suggesting a strong cool core, which is typically found at the centers of relaxed clusters. However, the large-scale morphology of CHIPS1911+4455 is highly asymmetric, pointing to a more dynamically active and turbulent cluster. Furthermore, the Hubble images reveal a massive, filamentary starburst near the brightest cluster galaxy (BCG). We measure the star formation rate for the BCG to be 140-190 M_⊙ yr^-1, which is one of the highest rates measured in a central cluster galaxy to date. One possible scenario for CHIPS1911+4455 is that the cool core was displaced during a major merger and rapidly cooled, with cool, star-forming gas raining back toward the core. This unique system is an excellent case study for high-redshift clusters, where such phenomena are proving to be more common. Further studies of such systems will drastically improve our understanding of the relation between cluster mergers and cooling, and how these fit in the bigger picture of active galactic nuclei feedback.

ID: 158864
Type: article
Authors: Bianchini, F.; Wu, W. L. K.; Ade, P. A. R.; Anderson, A. J.; Austermann, J. E.; Avva, J. S.; Balkenhol, L.; Baxter, E.; Beall, J. A.; Bender, A. N.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chaubal, P.; Chiang, H. C.; Chou, T. L.; Citron, R.; Corbett Moran, C.; Crawford, T. M.; Crites, A. T.; de Haan, T.; Dobbs, M. A.; Everett, W.; Gallicchio, J.; George, E. M.; Gilbert, A.; Gupta, N.; Halverson, N. W.; Henning, J. W.; Hilton, G. C.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; Knox, L.; Lee, A. T.; Li, D.; Lowitz, A.; Manzotti, A.; McMahon, J. J.; Meyer, S. S.; Millea, M.; Mocanu, L. M.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Noble, G.; Novosad, V.; Omori, Y.; Padin, S.; Patil, S.; Pryke, C.; Reichardt, C. L.; Ruhl, J. E.; Saliwanchik, B. R.; Schaffer, K. K.; Sievers, C.; Simard, G.; Smecher, G.; Stark, Antony A.; Story, K. T.; Tucker, C.; Vanderlinde, K.; Veach, T.; Vieira, J. D.; Wang, G.; Whitehorn, N.; Yefremenko, V.
Abstract: We present a search for anisotropic cosmic birefringence in 500 deg² of southern sky observed at 150 GHz with the SPTpol camera on the South Pole Telescope. We reconstruct a map of cosmic polarization rotation anisotropies using higher-order correlations between the observed cosmic microwave background (CMB) E and B fields. We then measure the angular power spectrum of this map, which is found to be consistent with zero. The nondetection is translated into an upper limit on the amplitude of the scale-invariant cosmic rotation power spectrum, L (L +1 )C_L^{a a}/2 p /2 p ^-4 rad² (0.033 deg² , 95% C.L.). This upper limit can be used to place constraints on the strength of primordial magnetic fields, B_{1 Mpca ?}^-2 /H_I (95% C.L.), where H_I is the inflationary Hubble scale. For the first time, we also cross-correlate the CMB temperature fluctuations with the reconstructed rotation angle map, a signal expected to be nonvanishing in certain theoretical scenarios, and find no detectable signal. We perform a suite of systematics and consistency checks and find no evidence for contamination.

ID: 155701
Type: article
Authors: Bianchini, F.; Wu, W. L. K.; Ade, P. A. R.; Anderson, A. J.; Austermann, J. E.; Avva, J. S.; Beall, J. A.; Bender, A. N.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chaubal, P.; Chiang, H. C.; Citron, R.; Moran, C. Corbett; Crawford, T. M.; Crites, A. T.; de Haan, T.; Dobbs, M. A.; Everett, W.; Gallicchio, J.; George, E. M.; Gilbert, A.; Gupta, N.; Halverson, N. W.; Harrington, N.; Henning, J. W.; Hilton, G. C.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; Knox, L.; Lee, A. T.; Li, D.; Lowitz, A.; Manzotti, A.; McMahon, J. J.; Meyer, S. S.; Millea, M.; Mocanu, L. M.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Noble, G.; Novosad, V.; Omori, Y.; Padin, S.; Patil, S.; Pryke, C.; Reichardt, C. L.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Schaffer, K. K.; Sievers, C.; Simard, G.; Smecher, G.; Stark, Antony A.; Story, K. T.; Tucker, C.; Vanderlinde, K.; Veach, T.; Vieira, J. D.; Wang, G.; Whitehorn, N.; Yefremenko, V.
Abstract: We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg² SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO), as well as primary CMB spectra from Planck and SPTpol. The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on ${\sigma }_{8}{{\rm{\Omega }}}_{m}^{0.25}=0.593\pm 0.025$ . Jointly fitting with BAO data, we find ${\sigma }_{8}=0.779\pm 0.023$ , ${{\rm{\Omega }}}_{m}={0.368}_{-0.037}^{+0.032}$ , and ${H}_{0}={72.0}_{-2.5}^{+2.1}\, \mathrm{km}\,{{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$ , up to $2\sigma $ away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be ${{\rm{\Omega }}}_{K}=-0.0007\pm 0.0025$ and the sum of the neutrino masses to be $\sum {m}_{\nu }\lt 0.23$ eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. With the differences in the signal-to-noise ratio of the lensing modes and the angular scales covered in the lensing spectra, this analysis represents an important independent check on the full-sky Planck lensing measurement.

ID: 156470
Type: article
Authors: Bleem, L. E.; Bocquet, S.; Stalder, Brian; Gladders, M. D.; Ade, P. A. R.; Allen, S. W.; Anderson, A. J.; Annis, J.; Ashby, Matthew L. N.; Austermann, J. E.; Avila, S.; Avva, J. S.; Bayliss, M.; Beall, J. A.; Bechtol, K.; Bender, A. N.; Benson, B. A.; Bertin, E.; Bianchini, F.; Blake, C.; Brodwin, M.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Carlstrom, J. E.; Rosell, A. Carnero; Carrasco Kind, M.; Carretero, J.; Chang, C. L.; Chiang, H. C.; Citron, R.; Moran, C. Corbett; Costanzi, M.; Crawford, T. M.; Crites, A. T.; da Costa, L. N.; de Haan, T.; De Vicente, J.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Dobbs, M. A.; Eifler, T. F.; Everett, W.; Flaugher, B.; Floyd, B.; Frieman, J.; Gallicchio, J.; García-Bellido, J.; George, E. M.; Gerdes, D. W.; Gilbert, A.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gupta, N.; Gutierrez, G.; Halverson, N. W.; Harrington, N.; Henning, J. W.; Heymans, C.; Holder, G. P.; Hollowood, D. L.; Holzapfel, W. L.; Honscheid, K.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; James, David J.; Jeltema, T.; Joudaki, S.; Khullar, G.; Klein, M.; Knox, L.; Kuropatkin, N.; Lee, A. T.; Li, D.; Lidman, C.; Lowitz, A.; MacCrann, N.; Mahler, G.; Maia, M. A. G.; Marshall, J. L.; McDonald, M.; McMahon, J. J.; Melchior, P.; Menanteau, F.; Meyer, S. S.; Miquel, R.; Mocanu, L. M.; Mohr, J. J.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Noble, G.; Novosad, V.; Padin, S.; Palmese, A.; Parkinson, D.; Patil, S.; Paz-Chinchón, F.; Plazas, A. A.; Pryke, C.; Ramachandra, N. S.; Reichardt, C. L.; Remolina González, J. D.; Romer, A. K.; Roodman, A.; Ruhl, J. E.; Rykoff, E. S.; Saliwanchik, B. R.; Sanchez, E.; Saro, A.; Sayre, J. T.; Schaffer, K. K.; Schrabback, T.; Serrano, S.; Sharon, K.; Sievers, C.; Smecher, G.; Smith, M.; Soares-Santos, M.; Stark, Antony A.; Story, K. T.; Suchyta, E.; Tarle, G.; Tucker, C.; Vanderlinde, K.; Veach, T.; Vieira, J. D.; Wang, G.; Weller, J.; Whitehorn, N.; Wu, W. L. K.; Yefremenko, V.; Zhang, Y.
Abstract: We describe the observations and resultant galaxy cluster catalog from the 2770 deg² SPTpol Extended Cluster Survey (SPT-ECS). Clusters are identified via the Sunyaev-Zel'dovich (SZ) effect and confirmed with a combination of archival and targeted follow-up data, making particular use of data from the Dark Energy Survey (DES). With incomplete follow-up we have confirmed as clusters 244 of 266 candidates at a detection significance ξ ≥ 5 and an additional 204 systems at 4 SPTpol Extended Cluster Survey (SPT-ECS). Clusters are identified via the Sunyaev-Zel'dovich (SZ) effect and confirmed with a combination of archival and targeted follow-up data, making particular use of data from the Dark Energy Survey (DES). With incomplete follow-up we have confirmed as clusters 244 of 266 candidates at a detection significance ξ ≥ 5 and an additional 204 systems at 4 SPTpol Extended Cluster Survey (SPT-ECS). Clusters are identified via the Sunyaev-Zel'dovich (SZ) effect and confirmed with a combination of archival and targeted follow-up data, making particular use of data from the Dark Energy Survey (DES). With incomplete follow-up we have confirmed as clusters 244 of 266 candidates at a detection significance ξ ≥ 5 and an additional 204 systems at 4 ¹⁴ M_{☉} h₇₀^-1 and a median redshift of z = 0.49, and we have identified 44 strong gravitational lenses in the sample thus far. Radio data are used to characterize contamination to the SZ signal; the median contamination for confirmed clusters is predicted to be ∼1% of the SZ signal at the ξ > 4 threshold, and 10% of their measured SZ flux. We associate SZ-selected clusters, from both SPT-ECS and the SPT-SZ survey, with clusters from the DES redMaPPer sample, and we find an offset distribution between the SZ center and central galaxy in general agreement with previous work, though with a larger fraction of clusters with significant offsets. Adopting a fixed Planck-like cosmology, we measure the optical richness-SZ mass (λ-M) relation and find it to be 28% shallower than that from a weak-lensing analysis of the DES data - a difference significant at the 4σ level - with the relations intersecting at λ = 60. The SPT-ECS cluster sample will be particularly useful for studying the evolution of massive clusters and, in combination with DES lensing observations and the SPT- SZ cluster sample, will be an important component of future cosmological analyses.

ID: 156235
Type: article
Authors: Chen, Ping; Dong, Subo; Stritzinger, M. D.; Holmbo, Simon; Strader, Jay; Kochanek, C. S.; Peng, Eric W.; Benetti, S.; Bersier, D.; Brownsberger, Sasha; Buckley, David A. H.; Gromadzki, Mariusz; Moran, Shane; Pastorello, A.; Aydi, Elias; Bose, Subhash; Connor, Thomas; Boutsia, K.; Mille, F. Di; Elias-Rosa, N.; French, K. Decker; Holoien, Thomas W. -S; Mattila, Seppo; Shappee, B. J.; Stark, Antony A.; Swihart, Samuel J.
Abstract: We report observations of the hydrogen-deficient supernova (SN) 2019bkc/ATLAS19dqr. With B- and r-band decline between peak and 10 days post peak of ${\rm{\Delta }}{m}_{10}(B)=5.24\pm 0.07$ mag and ${\rm{\Delta }}{m}_{10}(r)=3.85\pm 0.10$ mag, respectively, SN 2019bkc is the most rapidly declining SN I discovered so far. While its closest matches are the rapidly declining SN 2005ek and SN 2010X, the light curves and spectra of SN 2019bkc show some unprecedented characteristics. SN 2019bkc appears "hostless," with no identifiable host galaxy near its location, although it may be associated with the galaxy cluster MKW1 at z = 0.02. We evaluate a number of existing models of fast-evolving SNe, and we find that none of them can satisfactorily explain all aspects of SN 2019bkc observations.

ID: 157315
Type: article
Authors: Cunningham, D. J. M.; Chapman, S. C.; Aravena, M.; de Breuck, C.; Béthermin, M.; Chen, Chian-Chou; Dong, Chenxing; Gonzalez, A. H.; Greve, T. R.; Litke, K. C.; Ma, J.; Malkan, M.; Marrone, D. P.; Miller, T.; Phadke, K. A.; Reuter, C.; Rotermund, K.; Spilker, J. S.; Stark, Anthony A.; Strandet, M.; Vieira, J. D.; Weiß, A.
Abstract: We present Atacama Compact Array and Atacama Pathfinder Experiment observations of the [N II] 205 μm fine-structure line in 40 sub- millimetre galaxies lying at redshifts z = 3-6, drawn from the 2500 deg² South Pole Telescope survey. This represents the largest uniformly selected sample of high-redshift [N II] 205 μm measurements to date. 29 sources also have [C II] 158 μm line observations allowing a characterization of the distribution of the [C II] to [N II] luminosity ratio for the first time at high redshift. The sample exhibits a median L $_{{\rm{[C\,{\small II}]}}}$ /L $_{{\rm{[N\,{\small II}]}}}$ ≍ 11.0 and interquartile range of 5.0 -24.7. These ratios are similar to those observed in local (Ultra)luminous infrared galaxies (LIRGs), possibly indicating similarities in their interstellar medium. At the extremes, we find individual sub-millimetre galaxies with L $_{{\rm{[C\,{\small II}]}}}$ /L $_{{\rm{[N\,{\small II}]}}}$ low enough to suggest a smaller contribution from neutral gas than ionized gas to the [C II] flux and high enough to suggest strongly photon or X-ray region dominated flux. These results highlight a large range in this line luminosity ratio for sub-millimetre galaxies, which may be caused by variations in gas density, the relative abundances of carbon and nitrogen, ionization parameter, metallicity, and a variation in the fractional abundance of ionized and neutral interstellar medium.

ID: 157480
Type: article
Authors: Everett, W. B.; Zhang, L.; Crawford, T. M.; Vieira, J. D.; Aravena, M.; Archipley, M. A.; Austermann, J. E.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chapman, S.; Crites, A. T.; de Haan, T.; Dobbs, M. A.; George, E. M.; Halverson, N. W.; Harrington, N.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Knox, L.; Lee, A. T.; Luong-Van, D.; Mangian, A. C.; Marrone, D. P.; McMahon, J. J.; Meyer, S. S.; Mocanu, L. M.; Mohr, J. J.; Natoli, T.; Padin, S.; Pryke, C.; Reichardt, C. L.; Reuter, C. A.; Ruhl, J. E.; Sayre, J. T.; Schaffer, K. K.; Shirokoff, E.; Spilker, J. S.; Stalder, Brian; Staniszewski, Z.; Stark, Anthony A.; Story, K. T.; Switzer, E. R.; Vanderlinde, K.; Weiß, A.; Williamson, R.
Abstract: We present a catalog of emissive point sources detected in the SPT-SZ survey, a contiguous 2530 square degree area surveyed with the South Pole Telescope (SPT) from 2008-2011 in three bands centered at 95, 150, and 220 GHz. The catalog contains 4845 sources measured at a significance of 4.5σ or greater in at least one band, corresponding to detections above approximately 9.8, 5.8, and 20.4 mJy in 95, 150, and 220 GHz, respectively. The spectral behavior in the SPT bands is used for source classification into two populations based on the underlying physical mechanisms of compact, emissive sources that are bright at millimeter wavelengths: synchrotron radiation from active galactic nuclei and thermal emission from dust. The latter population includes a component of high-redshift sources often referred to as submillimeter galaxies (SMGs). In the relatively bright flux ranges probed by the survey, these sources are expected to be magnified by strong gravitational lensing. The survey also contains sources consistent with protoclusters, groups of dusty galaxies at high redshift undergoing collapse. We cross-match the SPT-SZ catalog with external catalogs at radio, infrared, and X-ray wavelengths and identify available redshift information. The catalog splits into 3980 synchrotron-dominated and 865 dust-dominated sources, and we determine a list of 506 SMGs. Ten sources in the catalog are identified as stars. We calculate number counts for the full catalog, and synchrotron and dusty components, using a bootstrap method and compare our measured counts with models. This paper represents the third and final catalog of point sources in the SPT-SZ survey.

ID: 157811
Type: article
Authors: Grandis, S.; Klein, M.; Mohr, J. J.; Bocquet, S.; Paulus, M.; Abbott, T. M. C.; Aguena, M.; Allam, S.; Annis, J.; Benson, B. A.; Bertin, E.; Bhargava, S.; Brooks, D.; Burke, D. L.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Capasso, R.; Costanzi, M.; da Costa, L. N.; De Vicente, J.; Desai, S.; Dietrich, J. P.; Doel, P.; Eifler, T. F.; Evrard, A. E.; Flaugher, B.; Fosalba, P.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Hartley, W. G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; James, David J.; Jeltema, T.; Kuehn, K.; Kuropatkin, N.; Lima, M.; Maia, M. A. G.; Marshall, J. L.; Melchior, P.; Menanteau, F.; Miquel, R.; Ogando, R. L. C.; Palmese, A.; Paz-Chinchón, F.; Plazas, A. A.; Romer, A. K.; Roodman, A.; Sanchez, E.; Saro, A.; Scarpine, V.; Schubnell, M.; Serrano, S.; Sheldon, E.; Smith, M.; Stark, Antony A.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; Tucker, D. L.; Varga, T. N.; Weller, J.; Wilkinson, R.
Abstract: We construct and validate the selection function of the MARD-Y3 galaxy cluster sample. This sample was selected through optical follow-up of the 2nd ROSAT faint source catalogue with Dark Energy Survey year 3 data. The selection function is modelled by combining an empirically constructed X-ray selection function with an incompleteness model for the optical follow-up. We validate the joint selection function by testing the consistency of the constraints on the X-ray flux-mass and richness-mass scaling relation parameters derived from different sources of mass information: (1) cross-calibration using South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) clusters, (2) calibration using number counts in X-ray, in optical and in both X-ray and optical while marginalizing over cosmological parameters, and (3) other published analyses. We find that the constraints on the scaling relation from the number counts and SPT-SZ cross-calibration agree, indicating that our modelling of the selection function is adequate. Furthermore, we apply a largely cosmology independent method to validate selection functions via the computation of the probability of finding each cluster in the SPT-SZ sample in the MARD-Y3 sample and vice versa. This test reveals no clear evidence for MARD-Y3 contamination, SPT-SZ incompleteness or outlier fraction. Finally, we discuss the prospects of the techniques presented here to limit systematic selection effects in future cluster cosmological studies.

ID: 157479
Type: article
Authors: Hernández-Martín, B.; Schrabback, T.; Hoekstra, H.; Martinet, N.; Hlavacek-Larrondo, J.; Bleem, L. E.; Gladders, M. D.; Stalder, Brian; Stark, Anthony A.; Bayliss, M.
Abstract: Weak lensing measurements suffer from well-known shear estimation biases, which can be partially corrected for with the use of image simulations. In this work we present an analysis of simulated images that mimic Hubble Space Telescope/Advance Camera for Surveys observations of high-redshift galaxy clusters, including cluster specific issues such as non-weak shear and increased blending. Our synthetic galaxies have been generated to have similar observed properties as the background-selected source samples studied in the real images. First, we used simulations with galaxies placed on a grid to determine a revised signal-to-noise-dependent (S/N_KSB) correction for multiplicative shear measurement bias, and to quantify the sensitivity of our KSB+ bias calibration to mismatches of galaxy or PSF properties between the real data and the simulations. Next, we studied the impact of increased blending and light contamination from cluster and foreground galaxies, finding it to be negligible for high-redshift (z > 0.7) clusters, whereas shear measurements can be affected at the ∼1% level for lower redshift clusters given their brighter member galaxies. Finally, we studied the impact of fainter neighbours and selection bias using a set of simulated images that mimic the positions and magnitudes of galaxies in Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) data, thereby including realistic clustering. While the initial SExtractor object detection causes a multiplicative shear selection bias of -0.028 ± 0.002, this is reduced to -0.016 ± 0.002 by further cuts applied in our pipeline. Given the limited depth of the CANDELS data, we compared our CANDELS-based estimate for the impact of faint neighbours on the multiplicative shear measurement bias to a grid-based analysis, to which we added clustered galaxies to even fainter magnitudes based on Hubble Ultra Deep Field data, yielding a refined estimate of ∼ - 0.013. Our sensitivity analysis suggests that our pipeline is calibrated to an accuracy of ∼0.015 once all corrections are applied, which is fully sufficient for current and near-future weak lensing studies of high-redshift clusters. As an application, we used it for a refined analysis of three highly relaxed clusters from the South Pole Telescope Sunyaev-Zeldovich survey, where we now included measurements down to the cluster core (r > 200 kpc) as enabled by our work. Compared to previously employed scales (r > 500 kpc), this tightens the cluster mass constraints by a factor 1.38 on average.

ID: 156384
Type: article
Authors: Huang, N.; Bleem, L. E.; Stalder, Brian; Ade, P. A. R.; Allen, S. W.; Anderson, A. J.; Austermann, J. E.; Avva, J. S.; Beall, J. A.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Bocquet, S.; Brodwin, M.; Carlstrom, J. E.; Chang, C. L.; Chiang, H. C.; Citron, R.; Moran, C. Corbett; Crawford, T. M.; Crites, A. T.; Haan, T. de; Dobbs, M. A.; Everett, W.; Floyd, B.; Gallicchio, J.; George, E. M.; Gilbert, A.; Gladders, M. D.; Guns, S.; Gupta, N.; Halverson, N. W.; Harrington, N.; Henning, J. W.; Hilton, G. C.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Hubmayr, J.; Irwin, K. D.; Khullar, G.; Knox, L.; Lee, A. T.; Li, D.; Lowitz, A.; McDonald, M.; McMahon, J. J.; Meyer, S. S.; Mocanu, L. M.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Noble, G.; Novosad, V.; Padin, S.; Patil, S.; Pryke, C.; Reichardt, C. L.; Ruhl, J. E.; Saliwanchik, B. R.; Saro, A.; Sayre, J. T.; Schaffer, K. K.; Sharon, K.; Sievers, C.; Smecher, G.; Stark, Antony A.; Story, K. T.; Tucker, C.; Vanderlinde, K.; Veach, T.; Vieira, J. D.; Wang, G.; Whitehorn, N.; Wu, W. L. K.; Yefremenko, V.
Abstract: We present a catalog of galaxy cluster candidates detected in 100 square degrees surveyed with the SPTpol receiver on the South Pole Telescope. The catalog contains 89 candidates detected with a signal-to-noise ratio greater than 4.6. The candidates are selected using the Sunyaev─Zel'dovich effect at 95 and 150 GHz. Using both space- and ground-based optical and infrared telescopes, we have confirmed 81 candidates as galaxy clusters. We use these follow-up images and archival images to estimate photometric redshifts for 66 galaxy clusters and spectroscopic observations to obtain redshifts for 13 systems. An additional two galaxy clusters are confirmed using the overdensity of near-infrared galaxies only and are presented without redshifts. We find that 15 candidates (18% of the total sample) are at redshift z ≥ 1.0, with a maximum confirmed redshift of ${z}_{\max }=1.38\pm 0.10$ . We expect this catalog to contain every galaxy cluster with ${M}_{500c}\gt 2.6\times {10}^{14}{M}_{\odot }{{h}}_{70}^{-1}$ and z > 0.25 in the survey area. The mass threshold is approximately constant above z = 0.25, and the complete catalog has a median mass of approximately ${M}_{500c}=2.7\times {10}^{14}{M}_{\odot }{{h}}_{70}^{-1}$ . Compared to previous SPT works, the increased depth of the millimeter-wave data (11.2 and 6.5 μK-arcmin at 95 and 150 GHz, respectively) makes it possible to find more galaxy clusters at high redshift and lower mass.

ID: 157610
Type: article
Authors: Kim, Jae-Young; Krichbaum, Thomas P.; Broderick, Avery E.; Wielgus, Maciek; Blackburn, Lindy; Gómez, José L.; Johnson, Michael D.; Bouman, Katherine L.; Chael, Andrew; Akiyama, Kazunori; Jorstad, Svetlana; Marscher, Alan P.; Issaoun, Sara; Janssen, Michael; Chan, Chi-kwan; Savolainen, Tuomas; Pesce, Dominic W.; Özel, Feryal; Alberdi, Antxon; Alef, Walter; Asada, Keiichi; Azulay, Rebecca; Baczko, Anne-Kathrin; Ball, David; Baloković, Mislav; Barrett, John; Bintley, Dan; Boland, Wilfred; Bower, Geoffrey C.; Bremer, Michael; Brinkerink, Christiaan D.; Brissenden, Roger; Britzen, Silke; Broguiere, Dominique; Bronzwaer, Thomas; Byun, Do-Young; Carlstrom, John E.; Chatterjee, Shami; Chatterjee, Koushik; Chen, Ming-Tang; Chen, Yongjun; Cho, Ilje; Christian, Pierre; Conway, John E.; Cordes, James M.; Crew, Geoffrey B.; Cui, Yuzhu; Davelaar, Jordy; De Laurentis, Mariafelicia; Deane, Roger; Dempsey, Jessica; Desvignes, Gregory; Dexter, Jason; Doeleman, Sheperd S.; Eatough, Ralph P.; Falcke, Heino; Fish, Vincent L.; Fomalont, Ed; Fraga-Encinas, Raquel; Friberg, Per; Fromm, Christian M.; Galison, Peter; Gammie, Charles F.; García, Roberto; Gentaz, Olivier; Georgiev, Boris; Goddi, Ciriaco; Gold, Roman; Gómez-Ruiz, Arturo I.; Gu, Minfeng; Gurwell, Mark; Hada, Kazuhiro; Hecht, Michael H.; Hesper, Ronald; Ho, Luis C.; Ho, Paul; Honma, Mareki; Huang, Chih-Wei L.; Huang, Lei; Hughes, David H.; Ikeda, Shiro; Inoue, Makoto; James, David J.; Jannuzi, Buell T.; Jeter, Britton; Jiang, Wu; Jimenez-Rosales, Alejandra; Jung, Taehyun; Karami, Mansour; Karuppusamy, Ramesh; Kawashima, Tomohisa; Keating, Garrett K.; Kettenis, Mark; Kim, Junhan; Kim, Jongsoo; Kino, Motoki; Koay, Jun Yi; Koch, Patrick M.; Koyama, Shoko; Kramer, Michael; Kramer, Carsten; Kuo, Cheng-Yu; Lauer, Tod R.; Lee, Sang-Sung; Li, Yan-Rong; Li, Zhiyuan; Lindqvist, Michael; Lico, Rocco; Liu, Kuo; Liuzzo, Elisabetta; Lo, Wen-Ping; Lobanov, Andrei P.; Loinard, Laurent; Lonsdale, Colin; Lu, Ru-Sen; MacDonald, Nicholas R.; Mao, Jirong; Markoff, Sera; Marrone, Daniel P.; Martí-Vidal, Iván; Matsushita, Satoki; Matthews, Lynn D.; Medeiros, Lia; Menten, Karl M.; Mizuno, Yosuke; Mizuno, Izumi; Moran, James M.; Moriyama, Kotaro; Moscibrodzka, Monika; Musoke, Gibwa; Müller, Cornelia; Nagai, Hiroshi; Nagar, Neil M.; Nakamura, Masanori; Narayan, Ramesh; Narayanan, Gopal; Natarajan, Iniyan; Neri, Roberto; Ni, Chunchong; Noutsos, Aristeidis; Okino, Hiroki; Olivares, Héctor; Ortiz-León, Gisela N.; Oyama, Tomoaki; Palumbo, Daniel C. M.; Park, Jongho; Patel, Nimesh; Pen, Ue-Li; Piétu, Vincent; Plambeck, Richard; PopStefanija, Aleksandar; Porth, Oliver; Prather, Ben; Preciado-López, Jorge A.; Psaltis, Dimitrios; Pu, Hung-Yi; Ramakrishnan, Venkatessh; Rao, Ramprasad; Rawlings, Mark G.; Raymond, Alexander W.; Rezzolla, Luciano; Ripperda, Bart; Roelofs, Freek; Rogers, Alan; Ros, Eduardo; Rose, Mel; Roshanineshat, Arash; Rottmann, Helge; Roy, Alan L.; Ruszczyk, Chet; Ryan, Benjamin R.; Rygl, Kazi L. J.; Sánchez, Salvador; Sánchez-Arguelles, David; Sasada, Mahito; Schloerb, F. Peter; Schuster, Karl-Friedrich; Shao, Lijing; Shen, Zhiqiang; Small, Des; Sohn, Bong Won; SooHoo, Jason; Tazaki, Fumie; Tiede, Paul; Tilanus, Remo P. J.; Titus, Michael; Toma, Kenji; Torne, Pablo; Trent, Tyler; Traianou, Efthalia; Trippe, Sascha; Tsuda, Shuichiro; van Bemmel, Ilse; van Langevelde, Huib Jan; van Rossum, Daniel R.; Wagner, Jan; Wardle, John; Ward-Thompson, Derek; Weintroub, Jonathan; Wex, Norbert; Wharton, Robert; Wong, George N.; Wu, Qingwen; Yoon, Doosoo; Young, André; Young, Ken; Younsi, Ziri; Yuan, Feng; Yuan, Ye-Fei; Zensus, J. Anton; Zhao, Guangyao; Zhao, Shan-Shan; Zhu, Ziyan; Algaba, Juan-Carlos; Allardi, Alexander; Amestica, Rodrigo; Anczarski, Jadyn; Bach, Uwe; Baganoff, Frederick K.; Beaudoin, Christopher; Benson, Bradford A.; Berthold, Ryan; Blanchard, Jay M.; Blundell, Ray; Bustamente, Sandra; Cappallo, Roger; Castillo-Domínguez, Edgar; Chang, Chih-Cheng; Chang, Shu-Hao; Chang, Song-Chu; Chen, Chung-Chen; Chilson, Ryan; Chuter, Tim C.; Rosado, Rodrigo Córdova; Coulson, Iain M.; Crowley, Joseph; Derome, Mark; Dexter, Matthew; Dornbusch, Sven; Dudevoir, Kevin A.; Dzib, Sergio A.; Eckart, Andreas; Eckert, Chris; Erickson, Neal R.; Everett, Wendeline B.; Faber, Aaron; Farah, Joseph R.; Fath, Vernon; Folkers, Thomas W.; Forbes, David C.; Freund, Robert; Gale, David M.; Gao, Feng; Geertsema, Gertie; Graham, David A.; Greer, Christopher H.; Grosslein, Ronald; Gueth, Frédéric; Haggard, Daryl; Halverson, Nils W.; Han, Chih-Chiang; Han, Kuo-Chang; Hao, Jinchi; Hasegawa, Yutaka; Henning, Jason W.; Hernández-Gómez, Antonio; Herrero-Illana, Rubén; Heyminck, Stefan; Hirota, Akihiko; Hoge, James; Huang, Yau-De; Violette Impellizzeri, C. M.; Jiang, Homin; John, David; Kamble, Atish; Keisler, Ryan; Kimura, Kimihiro; Kono, Yusuke; Kubo, Derek; Kuroda, John; Lacasse, Richard; Laing, Robert A.; Leitch, Erik M.; Li, Chao-Te; Lin, Lupin C. -C; Liu, Ching-Tang; Liu, Kuan-Yu; Lu, Li-Ming; Marson, Ralph G.; Martin-Cocher, Pierre L.; Massingill, Kyle D.; Matulonis, Callie; McColl, Martin P.; McWhirter, Stephen R.; Messias, Hugo; Meyer-Zhao, Zheng; Michalik, Daniel; Montaña, Alfredo; Montgomerie, William; Mora-Klein, Matias; Muders, Dirk; Nadolski, Andrew; Navarro, Santiago; Neilsen, Joseph; Nguyen, Chi H.; Nishioka, Hiroaki; Norton, Timothy; Nowak, Michael A.; Nystrom, George; Ogawa, Hideo; Oshiro, Peter; Oyama, Tomoaki; Parsons, Harriet; Peñalver, Juan; Phillips, Neil M.; Poirier, Michael; Pradel, Nicolas; Primiani, Rurik A.; Raffin, Philippe A.; Rahlin, Alexandra S.; Reiland, George; Risacher, Christopher; Ruiz, Ignacio; Sáez-Madaín, Alejandro F.; Sassella, Remi; Schellart, Pim; Shaw, Paul; Silva, Kevin M.; Shiokawa, Hotaka; Smith, David R.; Snow, William; Souccar, Kamal; Sousa, Don; Sridharan, Tirupati K.; Srinivasan, Ranjani; Stahm, William; Stark, Antony A.; Story, Kyle; Timmer, Sjoerd T.; Vertatschitsch, Laura; Walther, Craig; Wei, Ta-Shun; Whitehorn, Nathan; Whitney, Alan R.; Woody, David P.; Wouterloot, Jan G. A.; Wright, Melvin; Yamaguchi, Paul; Yu, Chen-Yu; Zeballos, Milagros; Zhang, Shuo; Ziurys, Lucy; Event Horizon Telescope Collaboration
Abstract: 3C 279 is an archetypal blazar with a prominent radio jet that show broadband flux density variability across the entire electromagnetic spectrum. We use an ultra-high angular resolution technique - global Very Long Baseline Interferometry (VLBI) at 1.3 mm (230 GHz) - to resolve the innermost jet of 3C 279 in order to study its fine-scale morphology close to the jet base where highly variable γ-ray emission is thought to originate, according to various models. The source was observed during four days in April 2017 with the Event Horizon Telescope at 230 GHz, including the phased Atacama Large Millimeter/submillimeter Array (ALMA), at an angular resolution of ∼20 μas (at a redshift of z = 0.536 this corresponds to ∼0.13 pc ∼ 1700 Schwarzschild radii with a black hole mass M_BH = 8 × 10⁸ M_☉). Imaging and model-fitting techniques were applied to the data to parameterize the fine-scale source structure and its variation. We find a multicomponent inner jet morphology with the northernmost component elongated perpendicular to the direction of the jet, as imaged at longer wavelengths. The elongated nuclear structure is consistent on all four observing days and across different imaging methods and model-fitting techniques, and therefore appears robust. Owing to its compactness and brightness, we associate the northern nuclear structure as the VLBI "core". This morphology can be interpreted as either a broad resolved jet base or a spatially bent jet. We also find significant day-to-day variations in the closure phases, which appear most pronounced on the triangles with the longest baselines. Our analysis shows that this variation is related to a systematic change of the source structure. Two inner jet components move non-radially at apparent speeds of ∼15 c and ∼20 c (∼1.3 and ∼1.7 μas day^-1, respectively), which more strongly supports the scenario of traveling shocks or instabilities in a bent, possibly rotating jet. The observed apparent speeds are also coincident with the 3C 279 large-scale jet kinematics observed at longer (cm) wavelengths, suggesting no significant jet acceleration between the 1.3 mm core and the outer jet. The intrinsic brightness temperature of the jet components are ≲10¹⁰ K, a magnitude or more lower than typical values seen at ≥7 mm wavelengths. The low brightness temperature and morphological complexity suggest that the core region of 3C 279 becomes optically thin at short (mm) wavelengths.
The data are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/640/A69 and at http://https://eventhorizontelescope.org/for-astronomers/data

ID: 156884
Type: article
Authors: Mahler, Guillaume; Sharon, Keren; Gladders, Michael D.; Bleem, Lindsey; Bayliss, Matthew B.; Calzadilla, Michael S.; Floyd, Benjamin; Khullar, Gourav; McDonald, Michael; Remolina González, Juan D.; Schrabback, Tim; Stark, Antony A.; van den Busch, Jan Luca
Abstract: We present an analysis of the mass distribution inferred from strong lensing by SPT-CL J0356-5337, a cluster of galaxies at redshift $z=1.0359$ revealed in the follow-up of the SPT-SZ clusters. The cluster has an Einstein radius of ${\theta }_{{\rm{E}}}\simeq $ 14″ for a source at z = 3 and a mass within 500 kpc of ${M}_{500\mathrm{kpc}}=4.0\pm 0.8\times {10}^{14}\,$ ${M}_{\odot }$ . Our spectroscopic identification of three multiply imaged systems ( $z=2.363$ , $z=2.364$ , and $z=3.048$), combined with HSTF606W-band imaging allows us to build a strong lensing model for this cluster with an rms of $\leqslant 0\buildrel{\prime\prime}\over{.} 3$ . Our modeling reveals a two- component mass distribution in the cluster. One mass component is dominated by the brightest cluster Galaxy and the other component, separated by ∼170 kpc, contains a group of eight red elliptical galaxies confined in a ∼9″ (∼70 kpc) diameter circle. We estimate the mass ratio between the two components to be between 1:1.25 and 1:1.58. In addition, spectroscopic data reveal that these two near-equal mass cores have only a small velocity difference of ∼300 km s^-1 between the two components. This small radial velocity difference suggests that most of the relative velocity takes place in the plane of the sky, and implies that SPT-CL J0356-5337 is a major merger with a small impact parameter seen face-on. We also assess the relative contributions of Galaxy-scale halos to the overall mass of the core of the cluster and find that within 800 kpc from the brightest cluster Galaxy about 27% of the total mass can be attributed to visible and dark matter associated with galaxies, whereas only 73% of the total mass in the core comes from cluster-scale dark matter halos.

ID: 158084
Type: article
Authors: Nadolski, A.; Vieira, J. D.; Sobrin, J. A.; Kofman, A. M.; Ade, P. A. R.; Ahmed, Z.; Anderson, A. J.; Avva, J. S.; Basu Thakur, R.; Bender, A. N.; Benson, B. A.; Bryant, L.; Carlstrom, J. E.; Carter, F. W.; Cecil, T. W.; Chang, C. L.; Cheshire, J. R.; Chesmore, G. E.; Cliche, J. F.; Cukierman, A.; de Haan, T.; Dierickx, Marion; Ding, J.; Dutcher, D.; Everett, W.; Farwick, J.; Ferguson, K. R.; Florez, L.; Foster, A.; Fu, J.; Gallicchio, J.; Gambrel, A. E.; Gardner, R. W.; Groh, J. C.; Guns, S.; Guyser, R.; Halverson, N. W.; Harke-Hosemann, A. H.; Harrington, N. L.; Harris, R. J.; Henning, J. W.; Holzapfel, W. L.; Howe, D.; Huang, N.; Irwin, K. D.; Jeong, O.; Jonas, M.; Jones, A.; Korman, M.; Kovac, J.; Kubik, D. L.; Kuhlmann, S.; Kuo, C. -L; Lee, A. T.; Lowitz, A. E.; McMahon, J.; Meier, J.; Meyer, S. S.; Michalik, D.; Montgomery, J.; Natoli, T.; Nguyen, H.; Noble, G. I.; Novosad, V.; Padin, S.; Pan, Z.; Paschos, P.; Pearson, J.; Posada, C. M.; Quan, W.; Rahlin, A.; Riebel, D.; Ruhl, J. E.; Sayre, J. T.; Shirokoff, E.; Smecher, G.; Stark, Antony A.; Stephen, J.; Story, K. T.; Suzuki, A.; Tandoi, C.; Thompson, K. L.; Tucker, C.; Vanderlinde, K.; Wang, G.; Whitehorn, N.; Yefremenko, V.; Yoon, K. W.; Young, M. R.
Abstract: We present two prescriptions for broadband (~77 - 252 GHz), millimeter-wave antireflection coatings for cryogenic, sintered polycrystalline aluminum oxide optics: one for large-format (700 mm diameter) planar and plano-convex elements, the other for densely packed arrays of quasi-optical elements, in our case 5 mm diameter half-spheres (called "lenslets"). The coatings comprise three layers of commercially-available, polytetrafluoroethylene-based, dielectric sheet material. The lenslet coating is molded to fit the 150 mm diameter arrays directly while the large-diameter lenses are coated using a tiled approach. We review the fabrication processes for both prescriptions then discuss laboratory measurements of their transmittance and reflectance. In addition, we present the inferred refractive indices and loss tangents for the coating materials and the aluminum oxide substrate. We find that at 150 GHz and 300 K the large-format coating sample achieves (97 +/- 2)% transmittance and the lenslet coating sample achieves (94 +/- 3)% transmittance.

ID: 158814
Type: article
Authors: Reuter, C.; Vieira, J. D.; Spilker, J. S.; Weiß, A.; Aravena, M.; Archipley, M.; Béthermin, M.; Chapman, S. C.; de Breuck, C.; Dong, C.; Everett, W. B.; Fu, J.; Greve, T. R.; Hayward, C. C.; Hill, R.; Hezaveh, Y.; Jarugula, S.; Litke, K.; Malkan, M.; Marrone, D. P.; Narayanan, D.; Phadke, K. A.; Stark, Antony A.; Strandet, M. L.
Abstract: The South Pole Telescope (SPT) has systematically identified 81 high-redshift, strongly gravitationally lensed, dusty star-forming galaxies (DSFGs) in a 2500 square degree cosmological millimeter-wave survey. We present the final spectroscopic redshift survey of this flux-limited (S_{870 µm} > 25 mJy) sample, initially selected at 1.4 mm. The redshift survey was conducted with the Atacama Large Millimeter/submillimeter Array across the 3 mm spectral window, targeting carbon monoxide line emission. By combining these measurements with ancillary data, the SPT sample is now spectroscopically complete, with redshifts spanning 1.9 > 25 mJy) sample, initially selected at 1.4 mm. The redshift survey was conducted with the Atacama Large Millimeter/submillimeter Array across the 3 mm spectral window, targeting carbon monoxide line emission. By combining these measurements with ancillary data, the SPT sample is now spectroscopically complete, with redshifts spanning 1.9 5, making this the largest sample of high-redshift DSFGs to date, and enabling the "high-redshift tail" of extremely luminous DSFGs to be measured. Though galaxy formation models struggle to account for the SPT redshift distribution, the larger sample statistics from this complete and well-defined survey will help inform future theoretical efforts.

ID: 157857
Type: article
Authors: Sayre, J. T.; Reichardt, C. L.; Henning, J. W.; Ade, P. A. R.; Anderson, A. J.; Austermann, J. E.; Avva, J. S.; Beall, J. A.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Chaubal, P.; Chiang, H. C.; Citron, R.; Corbett Moran, C.; Crawford, T. M.; Crites, A. T.; de Haan, T.; Dobbs, M. A.; Everett, W.; Gallicchio, J.; George, E. M.; Gilbert, A.; Gupta, N.; Halverson, N. W.; Harrington, N.; Hilton, G. C.; Holder, G. P.; Holzapfel, W. L.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; Knox, L.; Lee, A. T.; Li, D.; Lowitz, A.; McMahon, J. J.; Meyer, S. S.; Mocanu, L. M.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Noble, G.; Novosad, V.; Padin, S.; Patil, S.; Pryke, C.; Ruhl, J. E.; Saliwanchik, B. R.; Schaffer, K. K.; Sievers, C.; Smecher, G.; Stark, Antony A.; Tucker, C.; Vanderlinde, K.; Veach, T.; Vieira, J. D.; Wang, G.; Whitehorn, N.; Wu, W. L. K.; Yefremenko, V.; SPTpol Collaboration
Abstract: We report a B -mode power spectrum measurement from the cosmic microwave background (CMB) polarization anisotropy observations made using the SPTpol instrument on the South Pole Telescope. This work uses 500 deg² of SPTpol data, a five-fold increase over the last SPTpol B -mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: 52 of SPTpol data, a five-fold increase over the last SPTpol B -mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: 52 of SPTpol data, a five-fold increase over the last SPTpol B -mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: 52 of SPTpol data, a five-fold increase over the last SPTpol B -mode release. As a result, the bandpower uncertainties have been reduced by more than a factor of two, and the measurement extends to lower multipoles: 52 ^-71 , corresponding to a 18.1 σ detection of power. With a prior on the galactic dust from Planck, WMAP and BICEP2/Keck observations, the SPTpol B -mode data can be used to set an upper limit on the tensor-to-scalar ratio, r , corresponding to a 18.1 σ detection of power. With a prior on the galactic dust from Planck, WMAP and BICEP2/Keck observations, the SPTpol B -mode data can be used to set an upper limit on the tensor-to-scalar ratio, r _lens, the data prefer A_lens=1.17 ±0.13 . These data are currently the most precise measurements of B -mode power at ℓ>320 .

ID: 154149
Type: article
Authors: Abbott, T. M. C.; Abdalla, F. B.; Alarcon, A.; Allam, S.; Annis, J.; Avila, S.; Aylor, K.; Banerji, M.; Banik, N.; Baxter, E. J.; Bechtol, K.; Becker, M. R.; Benson, B. A.; Bernstein, G. M.; Bertin, E.; Bianchini, F.; Blazek, J.; Bleem, L. E.; Bridle, S. L.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Carlstrom, J. E.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Castander, F. J.; Cawthon, R.; Chang, C.; Chang, C. L.; Cho, H. -M; Choi, A.; Chown, R.; Crawford, T. M.; Crites, A. T.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; Davis, C.; de Haan, T.; DeRose, J.; Desai, S.; De Vicente, J.; Diehl, H. T.; Dietrich, J. P.; Dobbs, M. A.; Dodelson, S.; Doel, P.; Drlica-Wagner, A.; Eifler, T. F.; Elvin-Poole, J.; Everett, W. B.; Flaugher, B.; Fosalba, P.; Friedrich, O.; Frieman, J.; García-Bellido, J.; Gatti, M.; Gaztanaga, E.; George, E. M.; Gerdes, D. W.; Giannantonio, T.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Halverson, N. W.; Harrington, N. L.; Hartley, W. G.; Holder, G. P.; Hollowood, D. L.; Holzapfel, W. L.; Honscheid, K.; Hou, Z.; Hoyle, B.; Hrubes, J. D.; Huterer, D.; Jain, B.; James, David J.; Jarvis, M.; Jeltema, T.; Johnson, M. W. G.; Johnson, M. D.; Kent, S.; Kirk, D.; Knox, L.; Kokron, N.; Krause, E.; Kuehn, K.; Lahav, O.; Lee, A. T.; Leitch, E. M.; Li, T. S.; Lima, M.; Lin, H.; Luong-Van, D.; MacCrann, N.; Maia, M. A. G.; Manzotti, A.; Marrone, D. P.; Marshall, J. L.; Martini, P.; McMahon, J. J.; Menanteau, F.; Meyer, S. S.; Miquel, R.; Mocanu, L. M.; Mohr, J. J.; Muir, J.; Natoli, T.; Nicola, A.; Nord, B.; Omori, Y.; Padin, S.; Pandey, S.; Plazas, A. A.; Porredon, A.; Prat, J.; Pryke, C.; Rau, M. M.; Reichardt, C. L.; Rollins, R. P.; Romer, A. K.; Roodman, A.; Ross, A. J.; Rozo, E.; Ruhl, J. E.; Rykoff, E. S.; Samuroff, S.; Sánchez, C.; Sanchez, E.; Sayre, J. T.; Scarpine, V.; Schaffer, K. K.; Secco, L. F.; Serrano, S.; Sevilla-Noarbe, I.; Sheldon, E.; Shirokoff, E.; Simard, G.; Smith, M.; Soares-Santos, M.; Sobreira, F.; Staniszewski, Z.; Stark, Anthony A.; Story, K. T.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; Troxel, M. A.; Tucker, D. L.; Vanderlinde, K.; Vieira, J. D.; Vielzeuf, P.; Vikram, V.; Walker, A. R.; Wechsler, R. H.; Weller, J.; Williamson, R.; Wu, W. L. K.; Yanny, B.; Zahn, O.; Zhang, Y.; Zuntz, J.; DES; SPT Collaborations
Abstract: We perform a joint analysis of the auto and cross-correlations between three cosmic fields: the galaxy density field, the galaxy weak lensing shear field, and the cosmic microwave background (CMB) weak lensing convergence field. These three fields are measured using roughly 1300 sq. deg. of overlapping optical imaging data from first year observations of the Dark Energy Survey (DES) and millimeter-wave observations of the CMB from both the South Pole Telescope Sunyaev- Zel'dovich survey and Planck. We present cosmological constraints from the joint analysis of the two-point correlation functions between galaxy density and galaxy shear with CMB lensing. We test for consistency between these measurements and the DES-only two-point function measurements, finding no evidence for inconsistency in the context of flat Λ CDM cosmological models. Performing a joint analysis of five of the possible correlation functions between these fields (excluding only the CMB lensing autospectrum) yields S₈≡σ₈√{Ω_m/0.3 }=0.78 2_-0.025^+0.019 and Ω_m=0.26 0_-0.019^+0.029 . We test for consistency between these five correlation function measurements and the Planck-only measurement of the CMB lensing autospectrum, again finding no evidence for inconsistency in the context of flat Λ CDM models. Combining constraints from all six two-point functions yields S₈=0.77 6_-0.021^+0.014 and Ω_m=0.27 1_-0.016^+0.022 . These results provide a powerful test and confirmation of the results from the first year DES joint-probes analysis.

ID: 155151
Type: article
Authors: Bocquet, S.; Dietrich, J. P.; Schrabback, T.; Bleem, L. E.; Klein, M.; Allen, S. W.; Applegate, D. E.; Ashby, Matthew L. N.; Bautz, M.; Bayliss, M.; Benson, B. A.; Brodwin, M.; Bulbul, Esra; Canning, R. E. A.; Capasso, R.; Carlstrom, J. E.; Chang, C. L.; Chiu, I.; Cho, H. -M; Clocchiatti, A.; Crawford, T. M.; Crites, A. T.; de Haan, T.; Desai, S.; Dobbs, M. A.; Foley, R. J.; Forman, William R.; Garmire, G. P.; George, E. M.; Gladders, M. D.; Gonzalez, A. H.; Grandis, S.; Gupta, N.; Halverson, N. W.; Hlavacek-Larrondo, J.; Hoekstra, H.; Holder, G. P.; Holzapfel, W. L.; Hou, Z.; Hrubes, J. D.; Huang, N.; Jones, Christine; Khullar, G.; Knox, L.; Kraft, Ralph; Lee, A. T.; von der Linden, A.; Luong-Van, D.; Mantz, A.; Marrone, D. P.; McDonald, M.; McMahon, J. J.; Meyer, S. S.; Mocanu, L. M.; Mohr, J. J.; Morris, R. G.; Padin, S.; Patil, S.; Pryke, C.; Rapetti, D.; Reichardt, C. L.; Rest, A.; Ruhl, J. E.; Saliwanchik, B. R.; Saro, A.; Sayre, J. T.; Schaffer, K. K.; Shirokoff, E.; Stalder, Brian; Stanford, S. A.; Staniszewski, Z.; Stark, Antony A.; Story, K. T.; Strazzullo, V.; Stubbs, Christopher W.; Vanderlinde, K.; Vieira, J. D.; Vikhlinin, Alexey; Williamson, R.; Zenteno, A.
Abstract: We derive cosmological constraints using a galaxy cluster sample selected from the 2500 deg² SPT-SZ survey. The sample spans the redshift range 0.25 SPT-SZ survey. The sample spans the redshift range 0.25 5. The sample is supplemented with optical weak gravitational lensing measurements of 32 clusters with 0.29 5. The sample is supplemented with optical weak gravitational lensing measurements of 32 clusters with 0.29 5. The sample is supplemented with optical weak gravitational lensing measurements of 32 clusters with 0.29 5. The sample is supplemented with optical weak gravitational lensing measurements of 32 clusters with 0.29 5. The sample is supplemented with optical weak gravitational lensing measurements of 32 clusters with 0.29 _m = 0.276 ± 0.047, σ ₈ = 0.781 ± 0.037, and σ ₈(Ω_m/0.3)^0.2 = 0.766 ±0.025. The redshift evolutions of the X-ray Y _X-mass and M _gas-mass relations are both consistent with self-similar evolution to within 1σ. The mass slope of the Y _X-mass relation shows a 2.3σ deviation from self-similarity. Similarly, the mass slope of the M _gas-mass relation is steeper than self- similarity at the 2.5σ level. In a νwCDM cosmology, we measure the dark energy equation-of-state parameter w = -1.55 ± 0.41 from the cluster data. We perform a measurement of the growth of structure since redshift z ∼ 1.7 and find no evidence for tension with the prediction from general relativity. This is the first analysis of the SPT cluster sample that uses direct weak-lensing mass calibration and is a step toward using the much larger weak-lensing data set from DES. We provide updated redshift and mass estimates for the SPT sample.