Author: "Vásquez, J." - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Vásquez, J."' showing total 658 results

Start Over Author "Vásquez, J."

658 results on '"Vásquez, J."'

1. New JWST redshifts for the host galaxies of CDF-S XT1 and XT2: understanding their nature

Author: Quirola-Vásquez, J., Bauer, F. E., Jonker, P. G., Levan, A., Brandt, W. N., Ravasio, M., Eappachen, D., Xue, Y. Q., and Zheng, X. C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: CDF-S XT1 and XT2 are considered two "canonical" extragalactic fast X-ray transients (FXTs). In this work, we report new constraints on both FXTs, based on recent JWST NIRCam and MIRI photometry, as well as NIRspec spectroscopy for CDF-S XT2 that allow us to improve our understanding of their distances, energetics, and host galaxy properties compared to the pre-JWST era. We use the available HST and JWST archival data to determine the host properties and constrain the energetics of each FXT based on spectral energy distribution (SED) photometric fitting. The host of CDF-S XT1 is now constrained to lie at $z_{phot}{=}2.76_{-0.13}^{+0.21}$, implying a host absolute magnitude $M_{R}=-19.14$ mag, stellar mass $M_{*}$=2.8e8 $M_\odot$, and star formation rate SFR=0.62 $M_\odot$~yr$^{-1}$. These properties lie at the upper end of previous estimates, leaving CDF-S XT1 with a peak X-ray luminosity of $L_{X,peak}$=2.8e47 erg s$^{-1}$. We argue that the best progenitor scenario for XT1 is a low-luminosity gamma-ray burst (GRB), although we do not fully rule out a proto-magnetar association or a jetted tidal disruption event involving a white dwarf and an intermediate-massive black hole. In the case of CDF-S XT2, JWST imaging reveals a new highly obscured component of the host galaxy, previously missed by HST, while NIRspec spectroscopy securely places the host at $z_{spec}{=}3.4598{\pm}0.0022$. The new redshift implies a host with $M_{R}=-21.76$ mag, $M_{*}$=5.5e10 $M_\odot$, SFR=160 $M_\odot$ yr$^{-1}$, and FXT $L_{X,peak}$=1.4e47 erg s$^{-1}$. The revised energetics, similarity to X-ray flash event light curves, small host offset, and high host SFR favor a low-luminosity collapsar progenitor for CDF-S XT2. While these HST and JWST observations shed light on the host galaxies of XT1 and XT2, and by extension, on the nature of FXTs, a unique explanation for both sources remains elusive., Comment: The manuscript was submitted to Astronomy & Astrophysics in August 2024
Published: 2024

2. Investigating the off-axis GRB afterglow scenario for extragalactic fast X-ray transients

Author: Wichern, H. C. I., Ravasio, M. E., Jonker, P. G., Quirola-Vásquez, J. A., Levan, A. J., Bauer, F. E., and Kann, D. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Extragalactic fast X-ray transients (FXTs) are short-duration ($\sim$ ks) X-ray flashes of unknown origin, potentially arising from binary neutron star mergers. We investigate the possible link between FXTs and the afterglows of off-axis merger-induced gamma-ray bursts (GRBs). By modelling the broadband afterglows of 13 GRBs, we make predictions for their X-ray light curve behaviour had they been observed off-axis, considering both a uniform jet with core angle $\theta_{C}$ and a Gaussian-structured jet with truncation angle $\theta_{W} = 2\theta_{C}$. We compare their peak X-ray luminosity, duration, and temporal indices with those of the currently known extragalactic FXTs. Our analysis reveals that a slightly off-axis observing angle of $\theta_{\text{obs}}\approx (2.2-3)\theta_{C}$ and a structured jet are required to explain the shallow temporal indices of the FXT light curves. In the case of a structured jet, the durations of the FXTs are consistent with those of the off-axis afterglows for the same range of observing angles, $\theta_{\text{obs}}\approx (2.2-3)\theta_{C}$. While the off-axis peak X-ray luminosities are consistent only for $\theta_{\text{obs}} = 2.2\theta_{C}$, focussing on individual events reveals that the match of all three properties of the FXTs at the same viewing angle is possible in the range $\theta_{\text{obs}} \sim (2.2-2.6)\theta_{C}$. Despite the small sample of GRBs analysed, these results show that there is a region of the parameter space - although quite limited - where the observational properties of off-axis GRB afterglows can be consistent with those of the newly discovered FXTs. Future observations of FXTs discovered by the recently launched Einstein Probe mission and GRB population studies combined with more complex afterglow models will shed light on this possible GRB-FXT connection, and eventually unveil the progenitors of some FXTs., Comment: 24 pages, 7 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2024

3. Soft X-ray prompt emission from a high-redshift gamma-ray burst EP240315a

Author: Liu, Y., Sun, H., Xu, D., Svinkin, D. S., Delaunay, J., Tanvir, N. R., Gao, H., Zhang, C., Chen, Y., Wu, X. -F., Zhang, B., Yuan, W., An, J., Bruni, G., Frederiks, D. D., Ghirlanda, G., Hu, J. -W., Li, A., Li, C. -K., Li, J. -D., Malesani, D. B., Piro, L., Raman, G., Ricci, R., Troja, E., Vergani, S. D., Wu, Q. -Y., Yang, J., Zhang, B. -B., Zhu, Z. -P., Postigo, A. de Ugarte, Demin, A. G., Dobie, D., Fan, Z., Fu, S. -Y., Fynbo, J. P. U., Geng, J. -J., Gianfagna, G., Hu, Y. -D., Huang, Y. -F., Jiang, S. -Q., Jonker, P. G., Julakanti, Y., Kennea, J. A., Kokomov, A. A., Kuulkers, E., Lei, W. -H., Leung, J. K., Levan, A. J., Li, D. -Y., Li, Y., Littlefair, S. P., Liu, X., Lysenko, A. L., Ma, Y. -N., Martin-Carrillo, A., O'Brien, P., Parsotan, T., Quirola-Vasquez, J., Ridnaia, A. V., Ronchini, S., Rossi, A., Mata-Sanchez, D., Schneider, B., Shen, R. -F., Thakur, A. L., Tohuvavohu, A., Torres, M. A. P., Tsvetkova, A. E., Ulanov, M. V., Wei, J. -J., Xiao, D., Yin, Y. -H. I., Bai, M., Burwitz, V., Cai, Z. -M., Chen, F. -S., Chen, H. -L., Chen, T. -X., Chen, W., Chen, Y. -F., Chen, Y. -H., Cheng, H. -Q., Cui, C. -Z., Cui, W. -W., Dai, Y. -F., Dai, Z. -G., Eder, J., Fan, D. -W., Feldman, C., Feng, H., Feng, Z., Friedrich, P., Gao, X., Guan, J., Han, D. -W, Han, J., Hou, D. -J., Hu, H. -B., Hu, T., Huang, M. -H., Huo, J., Hutchinson, I., Ji, Z., Jia, S. -M., Jia, Z. -Q., Jiang, B. -W., Jin, C. -C., Jin, G., Jin, J. -J., Keereman, A., Lerman, H., Li, J. -F., Li, L. -H., Li, M. -S., Li, W., Li, Z. -D., Lian, T. -Y., Liang, E. -W., Ling, Z. -X., Liu, C. -Z., Liu, H. -Y., Liu, H. -Q., Liu, M. -J., Liu, Y. -R., Lu, F. -J., LU, H. -J., Luo, L. -D., Ma, F. L., Ma, J., Mao, J. -R., Mao, X., McHugh, M., Meidinger, N., Nandra, K., Osborne, J. P., Pan, H. -W., Pan, X., Ravasio, M. E., Rau, A., Rea, N., Rehman, U., Sanders, J., Santovincenzo, A., Song, L. -M., Su, J., Sun, L. -J., Sun, S. -L., Sun, X. -J., Tan, Y. -Y., Tang, Q. -J., Tao, Y. -H., Tong, J. -Z., Wang, H., Wang, J., Wang, L., Wang, W. -X., Wang, X. -F., Wang, X. -Y., Wang, Y. -L., Wang, Y. -S., Wei, D. -M., Willingale, R., Xiong, S. -L., Xu, H. -T., Xu, J. -J., Xu, X. -P., Xu, Y. -F., Xu, Z., Xue, C. -B., Xue, Y. -L., Yan, A. -L., Yang, F., Yang, H. -N., Yang, X. -T., Yang, Y. -J, Yu, Y. -W., Zhang, J., Zhang, M., Zhang, S. -N., Zhang, W. -D., Zhang, W. -J., Zhang, Y. -H., Zhang, Z., Zhang, Z. -L., Zhao, D. -H., Zhao, H. -S., Zhao, X. -F., Zhao, Z. -J., Zhou, L. -X., Zhou, Y. -L., Zhu, Y. -X., Zhu, Z. -C., and Zuo, X. -X.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Long gamma-ray bursts (GRBs) are believed to originate from core collapse of massive stars. High-redshift GRBs can probe the star formation and reionization history of the early universe, but their detection remains rare. Here we report the detection of a GRB triggered in the 0.5--4 keV band by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission, designated as EP240315a, whose bright peak was also detected by the Swift Burst Alert Telescope and Konus-Wind through off-line analyses. At a redshift of $z=4.859$, EP240315a showed a much longer and more complicated light curve in the soft X-ray band than in gamma-rays. Benefiting from a large field-of-view ($\sim$3600 deg$^2$) and a high sensitivity, EP-WXT captured the earlier engine activation and extended late engine activity through a continuous detection. With a peak X-ray flux at the faint end of previously known high-$z$ GRBs, the detection of EP240315a demonstrates the great potential for EP to study the early universe via GRBs., Comment: 41 pages, 8 figures, 7 tables
Published: 2024

4. The sPHENIX Micromegas Outer Tracker

Author: Aune, S., Azmoun, B., Bonenfant, A., Boose, S., Bregant, M., Cacace, D., da Silva, R. W., Feder, R., Francisco, A., Goblin, C., Grabas, A., Haggerty, J. S., Hernandez, R. A., Herrera, H. D. H., Huang, J., Kelsey, J., Kotov, I., Kuczewski, J., Mandjavidze, I., Martins, T. A., Mead, J., Mills, J., Oskarsson, A., Da Costa, H. Pereira, Pinkenburg, C., Pisani, R., Protzman, T., Purschke, M. L., Renner, E., Ruggiero, R., Sakaguchi, T., Sanches, B. C. S., Sayki, B., Silvermyr, D., Sondheim, W., Vandenbroucke, M., Van Noije, W. A. M., Vasquez, J., Vidal, C., and Wils, A.
Subjects: Physics - Instrumentation and Detectors
Abstract: The sPHENIX Time Projection Chamber Outer Tracker (TPOT) is a Micromegas based detector. It is a part of the sPHENIX experiment that aims to facilitate the calibration of the Time Projection Chamber, in particular the correction of the time-averaged and beam-induced distortions of the electron drift. This paper describes the detector mission, setup, construction, installation, commissioning and performance during the first year of sPHENIX data taking., Comment: 35 pages, 36 figures
Published: 2024
Full Text: View/download PDF

5. Probing a Magnetar Origin for the population of Extragalactic Fast X-ray Transients detected by Chandra

Author: Quirola-Vásquez, J., Bauer, F. E., Jonker, P. G., Brandt, W. N., Eappachen, D., Levan, A. J., Lopez, E., Luo, B., Ravasio, M. E., Sun, H., Xue, Y. Q., Yang, G., and Zheng, X. C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Twenty-two extragalactic fast X-ray transients (FXTs) have now been discovered from two decades of Chandra data (analyzing ~259 Ms of data), with 17 associated with distant galaxies (>100 Mpc). Different mechanisms and progenitors have been proposed to explain their properties; nevertheless, after analyzing their timing, spectral parameters, host-galaxy properties, luminosity function, and volumetric rates, their nature remains uncertain. We interpret a sub-sample of nine FXTs that show a plateau or a fast-rise light curve within the framework of a binary neutron star (BNS) merger magnetar model. We fit their light curves and derive magnetar (magnetic field and initial rotational period) and ejecta (ejecta mass and opacity) parameters. This model predicts two zones: an orientation-dependent free zone (where the magnetar spin-down X-ray photons escape freely to the observer) and a trapped zone (where the X-ray photons are initially obscured and only escape freely once the ejecta material becomes optically thin). We argue that six FXTs show properties consistent with the free zone and three FXTs with the trapped zone. This sub-sample of FXTs has a similar distribution of magnetic fields and initial rotation periods to those inferred for short gamma-ray bursts (SGRBs), suggesting a possible association. We compare the predicted ejecta emission fed by the magnetar emission (called merger-nova) to the optical and near-infrared upper limits of two FXTs, XRT 141001 and XRT 210423 where contemporaneous optical observations are available. The non-detections place lower limits on the redshifts of XRT 141001 and XRT 210423 of z>1.5 and >0.1, respectively. If the magnetar remnants lose energy via gravitational waves, it should be possible to detect similar objects with the current advanced LIGO detectors out to a redshift z<0.03, while future GW detectors will be able to detect them out to z=0.5., Comment: The paper was accepted for publication in Astronomy & Astrophysics
Published: 2024

6. Ethanol from Bagasse Obtained During Non-centrifuged Sugar Production. A Comprehensive Sustainability Analysis in the Colombian Context

Author: Piedrahita-Rodríguez, S., Ortiz-Sánchez, M., Higuita Vásquez, J. C., and Cardona Alzate, C. A.
Published: 2024
Full Text: View/download PDF

7. XMM-Newton-discovered Fast X-ray Transients: Host galaxies and limits on contemporaneous detections of optical counterparts

Author: Eappachen, D., Jonker, P. G., Quirola-Vásquez, J., Sánchez, D. Mata, Inkenhaag, A., Levan, A. J., Fraser, M., Torres, M. A. P., Bauer, F. E., Chrimes, A. A., Stern, D., Graham, M. J., Smartt, S. J., Smith, K. W., Ravasio, M. E., Zabludoff, A. I., Yue, M., Stoppa, F., Malesani, D. B., Stone, N. C., and Wen, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Extragalactic fast X-ray transients (FXTs) are a class of soft (0.3-10 keV) X-ray transients lasting a few hundred seconds to several hours. Several progenitor mechanisms have been suggested to produce FXTs, including supernova shock breakouts, binary neutron star mergers, or tidal disruptions involving an intermediate-mass black hole and a white dwarf. We present detailed host studies, including spectroscopic observations of the host galaxies of 7 XMM-Newton-discovered FXTs. The candidate hosts lie at redshifts 0.0928 $< z <$ 0.645 implying peak X-ray luminosities of 10$^{43}$ erg s$^{-1}$ $< L_X <$ 10$^{45}$ erg s$^{-1}$,and physical offsets of 1 kpc < $r_\mathrm{proj}$ < 22 kpc. These observations increase the number of FXTs with a spectroscopic redshift measurement by a factor of 2, although we note that one event is re-identified as a Galactic flare star. We infer host star formation rates and stellar masses by fitting the combined spectroscopic and archival photometric data. We also report on a contemporaneous optical counterpart search to the FXTs in Pan-STARRS and ATLAS by performing forced photometry at the position of the FXTs. We do not find any counterpart in our search. Given our constraints, including peak X-ray luminosities, optical limits, and host properties, we find that XRT 110621 is consistent with a SN SBO event. Spectroscopic redshifts of likely host galaxies for four events imply peak X-ray luminosities that are too high to be consistent with SN SBOs, but we are unable to discard either the BNS or WD-IMBH TDE scenarios for these FXTs., Comment: 17 pages, 10 figures, 6 tables. Accepted for publication in MNRAS
Published: 2023

8. Prospects for Time-Domain and Multi-Messenger Science with AXIS

Author: Time-Domain, The AXIS, Group, Multi-Messenger Science Working, Arcodia, Riccardo, Bauer, Franz E., Cenko, S. Bradley, Dage, Kristen C., Haggard, Daryl, Ho, Wynn C. G., Kara, Erin, Koss, Michael, Liu, Tingting, Mallick, Labani, Negro, Michela, Pradhan, Pragati, Quirola-Vasquez, J., Reynolds, Mark T., Ricci, Claudio, Rothschild, Richard E., Sridhar, Navin, Troja, Eleonora, and Yao, Yuhan
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Advanced X-ray Imaging Satellite (AXIS) promises revolutionary science in the X-ray and multi-messenger time domain. AXIS will leverage excellent spatial resolution (<1.5 arcsec), sensitivity (80x that of Swift), and a large collecting area (5-10x that of Chandra) across a 24-arcmin diameter field of view to discover and characterize a wide range of X-ray transients from supernova-shock breakouts to tidal disruption events to highly variable supermassive black holes. The observatory's ability to localize and monitor faint X-ray sources opens up new opportunities to hunt for counterparts to distant binary neutron star mergers, fast radio bursts, and exotic phenomena like fast X-ray transients. AXIS will offer a response time of <2 hours to community alerts, enabling studies of gravitational wave sources, high-energy neutrino emitters, X-ray binaries, magnetars, and other targets of opportunity. This white paper highlights some of the discovery science that will be driven by AXIS in this burgeoning field of time domain and multi-messenger astrophysics., Comment: This White Paper is part of a series commissioned for the AXIS Probe Concept Mission; additional AXIS White Papers can be found at http://axis.astro.umd.edu
Published: 2023

9. Proteomic profiling of Arabidopsis nuclei reveals distinct protein accumulation kinetics upon heat stress

Author: Muñoz-Díaz, E., Fuenzalida-Valdivia, I., Darrière, T., de Bures, A., Blanco-Herrera, F., Rompais, M., Carapito, C., and Sáez-Vásquez, J.
Published: 2024
Full Text: View/download PDF

10. Extragalactic FXT Candidates Discovered by Chandra (2014-2022)

Author: Quirola-Vásquez, J., Bauer, F. E., Jonker, P. G., Brandt, W. N., Yang, G., Levan, A. J., Xue, Y. Q., Eappachen, D., Camacho, E., Ravasio, M. E., Zheng, X. C., and Luo, B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Extragalactic fast X-ray transients (FXTs) are short flashes of X-ray photons of unknown origin that last a few minutes to hours. We extend the search for extragalactic FXTs from Quirola et al. 2022 (Paper I; based on sources in the Chandra Source Catalog 2.0, CSC2) to further Chandra archival data between 2014-2022. We extract X-ray data using a method similar to that employed by CSC2 and apply identical search criteria as in Paper I. We report the detection of eight FXT candidates, with peak 0.3-10 keV fluxes between 1$\times$10$^{-13}$ to 1$\times$10$^{-11}$ erg cm$^{-2}$ s$^{-1}$ and $T_{90}$ values from 0.3 to 12.1 ks. This sample of FXTs has likely redshifts between 0.7 to 1.8. Three FXT candidates exhibit light curves with a plateau (${\approx}$1-3 ks duration) followed by a power-law decay and X-ray spectral softening, similar to what was observed for a few previously reported FXTs in Paper I. In light of the new, expanded source lists (eight FXTs with known redshifts from Paper I and this work), we update the event sky rates derived in Paper I, finding 36.9$_{-8.3}^{+9.7}$ deg$^{-2}$ yr$^{-1}$ for the extragalactic samples for a limiting flux of ${\gtrsim}$1${\times}$10$^{-13}$ erg cm$^{-2}$ s$^{-1}$, calculate the first FXT X-ray luminosity function, and compare the volumetric density rate between FXTs and other transient classes. Our latest Chandra-detected extragalactic FXT candidates boost the total Chandra sample by $\sim$50 %, and appear to have a similar diversity of possible progenitors., Comment: 37 pages, 19 figures, 11 tables, accepted for publication in A&A. arXiv admin note: text overlap with arXiv:2201.07773
Published: 2023
Full Text: View/download PDF

11. Saturation and absorption effects on the transmission properties of Kerr-type nonlinear layers

Author: Betancur-Yepes, C. A., Mazo-Vásquez, J. D., and Reyes-Gómez, E.
Published: 2024
Full Text: View/download PDF

12. The Fast X-ray Transient XRT 210423 and its Host Galaxy

Author: Eappachen, D., Jonker, P. G., Levan, A. J., Quirola-Vasquez, J., Torres, M. A. P., Bauer, F. E., Dhillon, V. S., Marsh, T., Littlefair, S. P., Ravasio, M. E., and Fraser, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Fast X-ray Transients (FXTs) are X-ray flares with a duration ranging from a few hundred seconds to a few hours. Possible origins include the tidal disruption of a white dwarf by an intermediate-mass black hole, a supernova shock breakout, and a binary neutron star merger. We present the X-ray light curve and spectrum, and deep optical imaging of the FXT XRT 210423, which has been suggested to be powered by a magnetar produced in a binary neutron star merger. Our Very Large Telescope and Gran Telescopio Canarias (GTC) observations began on May 6, 2021, thirteen days after the onset of the flare. No transient optical counterpart is found in the 1" (3$\sigma$) X-ray uncertainty region of the source to a depth $g_{s}$=27.0 AB mag. A candidate host lies within the 1" X-ray uncertainty region with a magnitude of 25.9 $\pm$ 0.1 in the GTC/HiPERCAM $g_s$-filter. Due to its faintness, it was not detected in other bands, precluding a photometric redshift determination. We detect two additional candidate host galaxies; one with $z_{\rm spec}=1.5082 \pm 0.0001$ and an offset of 4.2$\pm$1" (37$\pm$9 kpc) from the FXT and another one with $z_{\rm phot}=1.04^{+0.22}_{-0.14}$, at an offset of 3.6$\pm$1" (30$\pm$8 kpc). Based on the properties of all the prospective hosts we favour a binary neutron star merger, as previously suggested in the literature, as explanation for XRT 210423., Comment: 14 pages, 6 figures. Accepted for publication in ApJ
Published: 2023
Full Text: View/download PDF

13. Panning for gold, but finding helium: discovery of the ultra-stripped supernova SN2019wxt from gravitational-wave follow-up observations

Author: Agudo, I., Amati, L., An, T., Bauer, F. E., Benetti, S., Bernardini, M. G., Beswick, R., Bhirombhakdi, K., de Boer, T., Branchesi, M., Brennan, S. J., Caballero-García, M. D., Cappellaro, E., Rodríguez, N. Castro, Castro-Tirado, A. J., Chambers, K. C., Chassande-Mottin, E., Chaty, S., Chen, T. -W., Coleiro, A., Covino, S., D'Ammando, F., D'Avanzo, P., D'Elia, V., Fiore, A., Flörs, A., Fraser, M., Frey, S., Frohmaier, C., Galbany, L., Gall, C., Gao, H., García-Rojas, J., Ghirlanda, G., Giarratana, S., Gillanders, J. H., Giroletti, M., Gompertz, B. P., Gromadzki, M., Heintz, K. E., Hu, Y. -D., Huber, M. E., Inkenhaag, A., Izzo, L., Jin, Z. P., Jonker, P. G., Kann, D. A., Kool, E. C., Kotak, R., Leloudas, G., Levan, A. J., Lin, C. -C., Lyman, J. D., Magnier, E. A., Maguire, K., Mandel, I., Marcote, B., Sánchez, D. Mata, Mattila, S., Melandri, A., Michałowski, M. J., Moldon, J., Nicholl, M., Guelbenzu, A. Nicuesa, Oates, S. R., Onori, F., Orienti, M., Paladino, R., Paragi, Z., Perez-Torres, M., Pian, E., Pignata, G., Piranomonte, S., Quirola-Vásquez, J., Ragosta, F., Rau, A., Ronchini, S., Rossi, A., Sánchez-Ramírez, R., Salafia, O. S., Schulze, S., Smartt, S. J., Smith, K. W., Sollerman, J., Srivastav, S., Starling, R. L. C., Steeghs, D., Stevance, H. F., Testa, V., Torres, M. A. P., Vergani, S. D., Vescovi, D., Wainscost, R., Watson, D., Wiersema, K., Wyrzykowski, Ł., Yang, J., Yang, S., and Young, D. R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the results from multi-wavelength observations of a transient discovered during the follow-up of S191213g, a gravitational wave (GW) event reported by the LIGO-Virgo Collaboration as a possible binary neutron star merger in a low latency search. This search yielded SN2019wxt, a young transient in a galaxy whose sky position (in the 80\% GW contour) and distance ($\sim$150\,Mpc) were plausibly compatible with the localisation uncertainty of the GW event. Initially, the transient's tightly constrained age, its relatively faint peak magnitude ($M_i \sim -16.7$\,mag) and the $r-$band decline rate of $\sim 1$\,mag per 5\,days appeared suggestive of a compact binary merger. However, SN2019wxt spectroscopically resembled a type Ib supernova, and analysis of the optical-near-infrared evolution rapidly led to the conclusion that while it could not be associated with S191213g, it nevertheless represented an extreme outcome of stellar evolution. By modelling the light curve, we estimated an ejecta mass of $\sim 0.1\,M_\odot$, with $^{56}$Ni comprising $\sim 20\%$ of this. We were broadly able to reproduce its spectral evolution with a composition dominated by helium and oxygen, with trace amounts of calcium. We considered various progenitors that could give rise to the observed properties of SN2019wxt, and concluded that an ultra-stripped origin in a binary system is the most likely explanation. Disentangling electromagnetic counterparts to GW events from transients such as SN2019wxt is challenging: in a bid to characterise the level of contamination, we estimated the rate of events with properties comparable to those of SN2019wxt and found that $\sim 1$ such event per week can occur within the typical GW localisation area of O4 alerts out to a luminosity distance of 500\,Mpc, beyond which it would become fainter than the typical depth of current electromagnetic follow-up campaigns., Comment: By the ENGRAVE collaboration (engrave-eso.org). 35 pages, 20 figures, final version accepted by A&A
Published: 2022
Full Text: View/download PDF

14. Probing for the host galaxies of the fast X-ray transients XRT 000519 and XRT 110103

Author: Eappachen, D., Jonker, P. G., Fraser, M., Torres, M. A. P., Dhillon, V. S., Marsh, T., Littlefair, S. P., Quirola-Vasquez, J., Maguire, K., Sanchez, D. Mata, Cannizzaro, G., Kostrzewa-Rutkowska, Z., Wevers, T., Onori, F., Inkenhaag, Anne, and Brennan, S. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: Over the past few years, $\sim$30 extragalactic fast X-ray transients (FXRTs) have been discovered, mainly in Chandra and XMM-Newton data. Their nature remains unclear, with proposed origins including a double neutron star merger, a tidal disruption event involving an intermediate-mass black hole and a white dwarf, or a supernova shock breakout. A decisive differentiation between these three promising mechanisms for their origin requires an understanding of the FXRT energetics, environments, and/or host properties. We present optical observations obtained with the Very Large Telescope for the FXRTs XRT 000519 and XRT 110103 and Gran Telescopio Canarias observations for XRT 000519 designed to search for host galaxies of these FXRTs. In the $g_s$, $r_s$ and $R$-band images, we detect an extended source on the North-West side of the $\sim$ $1^{\prime\prime}$ (68% confidence) error circle of the X-ray position of XRT 000519 with a Kron magnitude of $g_s=$26.29$\pm$0.09 (AB magnitude). We discuss the XRT 000519 association with the probable host candidate for various possible distances, and we conclude that if XRT 000519 is associated with the host candidate a supernova shock breakout scenario is likely excluded. No host galaxy is found near XRT 110103 down to a limiting magnitude of $R>25.8$., Comment: 11 pages, 11 figures, submitted to MNRAS
Published: 2022
Full Text: View/download PDF

15. Extragalactic fast X-ray transient candidates discovered by Chandra (2000-2014)

Author: Quirola-Vasquez, J., Bauer, F. E., Jonker, P. G., Brandt, W. N., Yang, G., Levan, A. J., Xue, Y. Q., Eappachen, D., Zheng, X. C., and Luo, B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Extragalactic Fast X-ray Transients (FXRTs) are short flashes of X-ray photons spanning a few seconds to hours, with an uncertain origin. Our ignorance about their physical mechanisms and progenitor systems is due in part to the lack of clear multi-wavelength counterparts in most cases because they only have been identified serendipitously. We develop a systematic search of FXRTs using a straightforward X-ray flare search algorithm, in the Chandra Source Catalog (Data Release 2.0; 169.6 Ms over 592.4 deg$^{2}$ using only observations with $|b|>10^{\circ}$ and before 2015), incorporating various multi-wavelength constraints to rule out Galactic contamination and characterize the candidates. We report the detection of 14 FXRT candidates from a parent sample of 214,701 sources. Candidates have peak 0.5-7 keV fluxes between 1$\times$10$^{-13}$ to 2$\times$10$^{-10}$ erg cm$^{-2}$ s$^{-1}$ and $T_{90}$ values from 4 to 48 ks. The sample can be subdivided into two groups: six "nearby" FXRTs that occurred within $d\lesssim$100 Mpc and eight "distant" FXRTs with likely redshifts $\gtrsim$0.1. Three distant FXRT candidates exhibit light curves with a plateau (${\approx}$1-3 ks duration) followed by a power-law decay and X-ray spectral softening, similar to what was observed for the previously reported FXRT CDF-S~XT2, a proposed magnetar-powered binary neutron star merger event. After applying completeness corrections, we calculate event rates for the nearby and distant samples of 53.7$_{-15.1}^{+22.6}$ and 28.2$_{-6.9}^{+9.8}$ deg$^{-2}$ yr$^{-1}$, respectively. This novel sample of Chandra-detected extragalactic FXRT candidates, although modest in size, breaks new ground in terms of characterizing the diverse properties, nature, and possible progenitors of these enigmatic events., Comment: 44 pages, 22 figures, submitted to A&A on Jan 6, 2022, and accepted on Apr 11, 2022
Published: 2022
Full Text: View/download PDF

16. Transmission of electromagnetic waves through nonlinear optical layers

Author: Hincapie-Zuluaga, L. M., Mazo-Vásquez, J. D., Betancur-Silvera, C. A., and Reyes-Gómez, E.
Subjects: Physics - Classical Physics
Abstract: The excitation of soliton states in optical layers exhibiting Kerr nonlinearities is theoretically investigated. The optical transmission coefficient is obtained as a function of the nonlinearity power of an incident monochromatic electromagnetic wave polarized in the transverse electric configuration. In materials exhibiting a defocusing nonlinearity, soliton excitations are not observed if the nonlinearity power associated with the incident electromagnetic wave is below a well-defined value. At such a limiting value of the nonlinearity power, a soliton excitation with an electric-field amplitude independent of the position is found within the nonlinear layer, regardless of the incident-wave frequency value.
Published: 2021
Full Text: View/download PDF

17. A Microwave SQUID Multiplexer Optimized for Bolometric Applications

Author: Dober, B., Ahmed, Z., Arnold, K., Becker, D. T., Bennett, D. A., Connors, J. A., Cukierman, A., D'Ewart, J. M., Duff, S. M., Dusatko, J. E., Frisch, J. C., Gard, J. D., Henderson, S. W., Herbst, R., Hilton, G. C., Hubmayr, J., Li, Y., Mates, J. A. B., McCarrick, H., Reintsema, C. D, Silva-Feaver, M., Ruckman, L., Ullom, J. N., Vale, L. R., Van Winkle, D. D., Vasquez, J., Wang, Y., Young, E., Yu, C., and Zheng, K.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: A microwave SQUID multiplexer ($\mu$MUX) has been optimized for coupling to large arrays of superconducting transition-edge sensor (TES) bolometers. We present the scalable cryogenic multiplexer chip design in a 1820-channel multiplexer configuration for the 4-8 GHz rf band. The key metrics of yield, sensitivity, and crosstalk are determined through measurements of 455 readout channels, which span 4-5 GHz. The median white-noise level is 45 pA/$\sqrt{\textrm{Hz}}$, evaluated at 2 Hz, with a 1/f knee $\leq$ 20 mHz after common-mode subtraction. The white-noise level decreases the sensitivity of a TES bolometer optimized for detection of the cosmic microwave background at 150 GHz by only 3%. The measured crosstalk between any channel pair is $\leq$ 0.3%., Comment: 6 pages, 5 figures
Published: 2020
Full Text: View/download PDF

18. Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv

Author: Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, M., Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, T. -W., Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F. I., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., González-Fernández, C., González-Gaitán, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutiérrez, C. P., Heikkilä, T., Heintz, K. E., Hjorth, J., Hu, Y. -D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, A., Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, E. C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michałowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Guelbenzu, A. Nicuesa, Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vásquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, S., Sabha, N. B., Carracedo, A. Sagués, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, T., Smartt, S. J., Smith, K. W., Smith, M., Sollerman, J., Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, S., Yi, S. -X., and Young, D. R.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. Preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope (ENGRAVE) collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical/near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS and VINROUGE projects also carried out a search on this event. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN) possibly generated by this NS-BH merger, and for the strategy of future searches. Altogether, our observations allow us to exclude a KN with large ejecta mass $M\gtrsim 0.1\,\mathrm{M_\odot}$ to a high ($>90\%$) confidence, and we can exclude much smaller masses in a subsample of our observations. This disfavours the tidal disruption of the neutron star during the merger. Despite the sensitive instruments involved in the campaign, given the distance of S190814bv we could not reach sufficiently deep limits to constrain a KN comparable in luminosity to AT 2017gfo on a large fraction of the localisation probability. This suggests that future (likely common) events at a few hundreds Mpc will be detected only by large facilities with both high sensitivity and large field of view. Galaxy-targeted observations can reach the needed depth over a relevant portion of the localisation probability with a smaller investment of resources, but the number of galaxies to be targeted in order to get a fairly complete coverage is large, even in the case of a localisation as good as that of this event., Comment: 52 pages, revised version now accepted for publication in A&A. Abstract abridged to meet arXiv requirements
Published: 2020
Full Text: View/download PDF

19. The Exceptional X-ray Evolution of SN1996cr in High Resolution

Author: Quirola-Vasquez, J., Bauer, F. E., Dwarkadas, V. V., Badenes, C., Brandt, W. N., Nymark, T., and Walton, D.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present X-ray spectra spanning 18 years of evolution for SN\,1996cr, one of the five nearest SNe detected in the modern era. {\it Chandra} HETG exposures in 2000, 2004, and 2009 allow us to resolve spectrally the velocity profiles of Ne, Mg, Si, S, and Fe emission lines and monitor their evolution as tracers of the ejecta-circumstellar medium (CSM) interaction. To explain the diversity of X-ray line profiles, we explore several possible geometrical models. Based on the highest signal-to-noise 2009 epoch, we find that a polar geometry with two distinct opening angle configurations and internal obscuration can successfully reproduce all of the observed line profiles. The best fit model consists of two plasma components: (1) a mildly absorbed (2$\times$10$^{21}$\,cm$^{-2}$), cooler ($\approx$2\,keV) with high Ne, Mg, Si, and S abundances associated with a wide polar interaction region (half-opening angle $\approx$58$^{\circ}$); (2) a moderately absorbed (2$\times$10$^{22}$\,cm$^{-2}$), hotter (>~20\,keV) plasma with high Fe abundances and strong internal obscuration associated with a narrow polar interaction region (half-opening angle $\approx$20$^{\circ}$). We extend this model to seven further epochs with lower signal-to-noise ratio and/or lower spectral-resolution between 2000-2018, yielding several interesting trends in absorption, flux, geometry and expansion velocity. We argue that the hotter and colder components are associated with reflected and forward shocks, respectively, at least at later epochs. We discuss the physical implications of our results and plausible explosion scenarios to understand the X-ray data of SN\,1996cr., Comment: 27 pages, 16 figures (+2 figures in the appendix), accepted for publication MNRAS
Published: 2019
Full Text: View/download PDF

20. Experimental Tests

Author: Sciumè, G., Riva Sanseverino, E., Gallo, P., Montana, F., Longo, S., Palacios-García, E. J., Vasquez, J. C., Guerrero, J. M., Riva Sanseverino, Eleonora, Editor-in-Chief, Amenta, Carlo, Series Editor, Carapezza, Marco, Series Editor, Chiodi, Marcello, Series Editor, Laghi, Andrea, Series Editor, Maresca, Bruno, Series Editor, Micale, Giorgio Domenico Maria, Series Editor, Mocciaro Li Destri, Arabella, Series Editor, Öchsner, Andreas, Series Editor, Piva, Mariacristina, Series Editor, Russo, Antonio, Series Editor, Seel, Norbert M., Series Editor, Sciumè, Giuseppe, editor, and Gallo, Pierluigi, editor
Published: 2022
Full Text: View/download PDF

21. Introduction

Author: Sciumè, G., Riva Sanseverino, E., Gallo, P., Di Silvestre, M. L., Zizzo, G., Musca, R., Vasquez, J. C., Guerrero, J. M., Riva Sanseverino, Eleonora, Editor-in-Chief, Amenta, Carlo, Series Editor, Carapezza, Marco, Series Editor, Chiodi, Marcello, Series Editor, Laghi, Andrea, Series Editor, Maresca, Bruno, Series Editor, Micale, Giorgio Domenico Maria, Series Editor, Mocciaro Li Destri, Arabella, Series Editor, Öchsner, Andreas, Series Editor, Piva, Mariacristina, Series Editor, Russo, Antonio, Series Editor, Seel, Norbert M., Series Editor, Sciumè, Giuseppe, editor, and Gallo, Pierluigi, editor
Published: 2022
Full Text: View/download PDF

22. Stability Analysis Using the Finite Element Method of a Slope in the Virgen de Fátima Sector of the San Juan de Lurigancho District of Lima, Peru

Author: Carrizales, N., Rodriguez, R., Vasquez, J., di Prisco, Marco, Series Editor, Chen, Sheng-Hong, Series Editor, Vayas, Ioannis, Series Editor, Kumar Shukla, Sanjay, Series Editor, Sharma, Anuj, Series Editor, Kumar, Nagesh, Series Editor, Wang, Chien Ming, Series Editor, Kang, Thomas, editor, and Lee, Youngjin, editor
Published: 2022
Full Text: View/download PDF

23. Modifying the native aluminum oxide layer by simple methods for fabricating write-once-read-many memory devices

Author: Portillo-Rodríguez, B., Sánchez-Vásquez, J. D., Reyes-Reyes, M., and López-Sandoval, R.
Published: 2023
Full Text: View/download PDF

24. Resistive organic memory devices based on nitrogen-doped CNTs/PSS composites

Author: Sánchez-Vásquez, J. D., Portillo-Rodríguez, B., Tovar-Martínez, E., Reyes-Reyes, M., and López-Sandoval, R.
Published: 2022
Full Text: View/download PDF

25. A submillimeter study of the IR dust bubble S 21 and its environs

Author: Cappa, C. E., Duronea, N. U., Vasquez, J., Rubio, M., Firpo, V., López-Caraballo, C. -H., and Borissova, J.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Based on the molecular emission in the $^{12}$CO(2-1) and $^{13}$CO(2-1) lines, and the continuum emission in the MIR and FIR towards the S21 IR dust bubble, we analyze the physical characteristics of the gas and dust linked to the nebula and the presence of young stellar objects (YSOs) in its environs. The line emission reveals a clumpy molecular shell, 1.4 pc in radius, encircling S21. The total molecular mass in the shell amounts to 2900 solar masses and the original ambient density, 2.1 x 10$^3$ cm$^{-3}$, indicating that the bubble is evolving in a high density interstellar medium. The image at 24 $\mu$m shows warm dust inside the bubble, while the emission in the range 250 to 870 $\mu$m reveal cold dust in its outskirts, coincident with the molecular gas. The detection of radio continuun emission indicates that the bubble is a compact HII region. A search for YSOs using photometric criteria allowed to identify many candidates projected onto the molecular clumps. We analize if the collect and collapse process has triggered a new generation of stars., Comment: 24 pages, 10 figures. Accepted for publication in RMxAC
Published: 2016

26. Molecular gas in the star-forming region IRAS 08589-4714

Author: Saldaño, Hugo P., Vásquez, J., Cappa, C. E., Gómez, M., Duronea, N. U., and Rubio, M.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present an analysis of the region IRAS 08589-4714 with the aim of characterizing the molecular environment. We observed the CO(3-2), ^{13}CO(3-2), C^{18}O(3-2), HCO+(3-2), and HCN(3-2) molecular lines in a region of 150" x 150", centered on the IRAS source, to analyze the distribution and characteristics of the molecular gas linked to the IRAS source. The molecular gas distribution reveals a molecular clump that is coincident with IRAS 08589-4714 and with a dust clump detected at 1.2 mm. The molecular clump is 0.45 pc in radius and its mass and H_2 volume density are 310 Mo and 1.2 x 10^4 cm^{-3}, respectively. Two overdensities were identified within the clump in HCN and HCO lines. A comparison of the LTE and virial masses suggests that the clump is collapsing in regions that harbor young stellar objects. An analysis of the molecular lines suggests that they are driving molecular outflows., Comment: 4 pages, 4 figures. Accepted for publication in A&A
Published: 2016
Full Text: View/download PDF

27. The IRAS 08589-4714 star-forming region

Author: Saldaño, H. P., Vásquez, J., Gómez, M., Cappa, C. E., Duronea, N. U., and Rubio, M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present an analysis of the IRAS 08589-4714 star-forming region. This region harbors candidate young stellar objects identified in the WISE and Herschel images using color index criteria and spectral energy distributions (SEDs). The SEDs of some of the infrared sources and the 70 microns radial intensity profile of the brightest source (IRS 1) are modeled from Herschel fluxes using the one-dimensional radiative transfer DUSTY code. For these objects, we estimate the envelope masses, sizes, densities, and luminosities which suggest that they are very young, massive and luminous objects at early stages of the formation process. Color-color diagrams in the bands of WISE and 2MASS are used to identify potential young objects in the region. Those identified in the bands of WISE would be contaminated by the emission of PAHs. We use the emission distribution in the infrared at 70 and 160 microns, to estimate the dust temperature gradient. This suggests that the nearby massive star-forming region RCW 38, located ~ 10 pc of the IRAS source position may be contributing to the photodissociation of the molecular gas and to the heating of the interstellar dust in the environs of the IRAS source., Comment: Accepted for publication in RMxAC
Published: 2016

28. Performance of a reinforced concrete wall building subjected to sequential earthquake and tsunami loading

Author: Tagle, S.J., Jünemann, R., Vásquez, J., de la Llera, J.C., and Baiguera, M.
Published: 2021
Full Text: View/download PDF

29. XMM-Newton-discovered Fast X-ray Transients:host galaxies and limits on contemporaneous detections of optical counterparts

Author: Eappachen, D, Jonker, P G, Quirola-vásquez, J, Sánchez, D Mata, Inkenhaag, A, Levan, A J, Fraser, M, Torres, M A P, Bauer, F E, Chrimes, A A, Stern, D, Graham, M J, Smartt, S J, Smith, K W, Ravasio, M E, Zabludoff, A I, Yue, M, Stoppa, F, Malesani, D B, Stone, N C, Wen, S, Eappachen, D, Jonker, P G, Quirola-vásquez, J, Sánchez, D Mata, Inkenhaag, A, Levan, A J, Fraser, M, Torres, M A P, Bauer, F E, Chrimes, A A, Stern, D, Graham, M J, Smartt, S J, Smith, K W, Ravasio, M E, Zabludoff, A I, Yue, M, Stoppa, F, Malesani, D B, Stone, N C, and Wen, S
Published: 2024

30. Molecular gas and star formation towards the IR dust bubble S24 and its environs

Author: Cappa, C. E., Duronea, N. U., Firpo, V., Vasquez, J., López-Caraballo, C. H., Rubio, M., and Vazzano, M. M.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present a multi-wavelength analysis of the infrared dust bubble S24, and its environs, with the aim of investigating the characteristics of the molecular gas and the interstellar dust linked to them, and analyzing the evolutionary status of the young stellar objects (YSOs) identified there. Using APEX data, we mapped the molecular emission in the CO(2-1), $^{13}$CO(2-1), C$^{18}$O(2-1), and $^{13}$CO(3-2) lines in a region of about 5'x 5' in size around the bubble. The cold dust distribution was analyzed using ATLASGAL and Herschel images. Complementary IR and radio data were also used.The molecular gas linked to the S24 bubble, G341.220-0.213, and G341.217-0.237 has velocities between -48.0 km sec$^{-1}$ and -40.0 km sec$^{-1}$. The gas distribution reveals a shell-like molecular structure of $\sim$0.8 pc in radius bordering the bubble. A cold dust counterpart of the shell is detected in the LABOCA and Herschel images.The presence of extended emission at 24 $\mu$m and radio continuum emission inside the bubble indicates that the bubble is a compact HII region. Part of the molecular gas bordering S24 coincides with the extended infrared dust cloud SDC341.194-0.221. A cold molecular clump is present at the interface between S24 and G341.217-0.237. As regards G341.220-0.213, the presence of an arc-like molecular structure at the northern and eastern sections of this IR source indicates that G341.220-0.213 is interacting with the molecular gas. Several YSO candidates are found to be linked to the IR extended sources, thus confirming their nature as active star-forming regions. The total gas mass in the region and the H$_2$ ambient density amount to 10300 M$_{\odot}$ and 5900 cm$^{-3}$, indicating that G341.220-0.213, G341.217-0.237, and the S24 HII region are evolving in a high density medium. A triggering star formation scenario is also investigated., Comment: 17 pages, 16 figures. Submitted to A&A. Revised according to the referee report
Published: 2015
Full Text: View/download PDF

31. 870 micron continuum observations of the bubble-shaped nebula Gum 31

Author: Duronea, N. U., Vasquez, J., Gómez, L., Cappa, C. E., Firpo, V., López-Carballo, C. H., and Rubio, M.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We are presenting here a study of the cold dust in the infrared ring nebula Gum 31. We aim at deriving the physical properties of the molecular gas and dust associated with the nebula, and investigating its correlation with the star formation in the region, that was probably triggered by the expansion of the ionization front. We use 870 micron data obtained with LABOCA to map the dust emission. The obtained LABOCA image was compared to archival IR,radio continuum, and optical images. The 870 micron emission follows the 8 micron (Spitzer), 250 micron, and 500 micron (Herschel) emission distributions showing the classical morphology of a spherical shell. We use the 870 micron and 250 micron images to identify 60 dust clumps in the collected layers of molecular gas using the Gaussclumps algorithm. The clumps have effective deconvolved radii between 0.16 pc and 1.35 pc, masses between 70 Mo and 2800 Mo, and volume densities between 1.1x10^3 cm^-3 and 2.04x10^5 cm^-3. The total mass of the clumps is 37600 Mo. The dust temperature of the clumps is in the range from 21 K to 32 K, while inside the HII region reaches ~ 40 K. The clump mass distribution is well-fitted by a power law dN/dlog(M/Mo) proportional to M^(-alpha), with alpha=0.93+/-0.28. The slope differs from those obtained for the stellar IMF in the solar neighborhood, suggesting that the clumps are not direct progenitors of single stars/protostars. The mass-radius relationship for the 41 clumps detected in the 870 microns emission shows that only 37% of them lie in or above the high-mass star formation threshold, most of them having candidate YSOs projected inside. A comparison of the dynamical age of the HII region with the fragmentation time, allowed us to conclude that the collect and collapse mechanism may be important for the star formation at the edge of Gum 31, although other processes may also be acting., Comment: 15 pages, 10 figures. Accepted for publication in A&A
Published: 2015
Full Text: View/download PDF

32. Prospects for Time-Domain and Multi-Messenger Science with AXIS.

Author: Arcodia, Riccardo, Bauer, Franz E., Cenko, S. Bradley, Dage, Kristen C., Haggard, Daryl, Ho, Wynn C. G., Kara, Erin, Koss, Michael, Liu, Tingting, Mallick, Labani, Negro, Michela, Pradhan, Pragati, Quirola-Vásquez, J., Reynolds, Mark T., Ricci, Claudio, Rothschild, Richard E., Sridhar, Navin, Troja, Eleonora, and Yao, Yuhan
Subjects: X-ray astronomy, SUPERMASSIVE black holes, GRAVITATIONAL waves, SOLAR radio bursts, X-ray binaries, X-ray imaging, SOFT X rays, NEUTRINOS
Abstract: The Advanced X-ray Imaging Satellite (AXIS) promises revolutionary science in the X-ray and multi-messenger time domain. AXIS will leverage excellent spatial resolution (<1.5 arcsec), sensitivity ( 80 × that of Swift), and a large collecting area (5–10× that of Chandra) across a 24-arcmin diameter field of view at soft X-ray energies (0.3–10.0 keV) to discover and characterize a wide range of X-ray transients from supernova-shock breakouts to tidal disruption events to highly variable supermassive black holes. The observatory's ability to localize and monitor faint X-ray sources opens up new opportunities to hunt for counterparts to distant binary neutron star mergers, fast radio bursts, and exotic phenomena like fast X-ray transients. AXIS will offer a response time of <2 h to community alerts, enabling studies of gravitational wave sources, high-energy neutrino emitters, X-ray binaries, magnetars, and other targets of opportunity. This white paper highlights some of the discovery science that will be driven by AXIS in this burgeoning field of time domain and multi-messenger astrophysics. This White Paper is part of a series commissioned for the AXIS Probe Concept Mission; additional AXIS White Papers can be found at the AXIS website. [ABSTRACT FROM AUTHOR]
Published: 2024
Full Text: View/download PDF

33. Analysis of a laboratory scale thermal energy accumulator using two-phases heterogeneous paraffin wax-water mixtures

Author: Reyes, A., Henríquez-Vargas, L., Vásquez, J., Pailahueque, N., and Aguilar, G.
Published: 2020
Full Text: View/download PDF

34. Probing a magnetar origin for the population of extragalactic fast X-ray transients detected by Chandra

Author: Quirola-Vásquez, J., primary, Bauer, F. E., additional, Jonker, P. G., additional, Brandt, W. N., additional, Eappachen, D., additional, Levan, A. J., additional, López, E., additional, Luo, B., additional, Ravasio, M. E., additional, Sun, H., additional, Xue, Y. Q., additional, Yang, G., additional, and Zheng, X. C., additional
Published: 2024
Full Text: View/download PDF

35. Molecular gas associated with IRAS 10361-5830

Author: Vazzano, M. M., Cappa, C. E., Vasquez, J., Rubio, M., and Romero, G. A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We analyze the distribution of the molecular gas and the dust in the molecular clump linked to IRAS 10361-5830, located in the environs of the bubble-shaped HII region Gum 31 in the Carina region, with the aim of determining the main parameters of the associated material and investigating the evolutionary state of the young stellar objects identified there. Using the APEX telescope, we mapped the molecular emission in the J=3-2 transition of three CO isotopologues, 12CO, 13CO and C18O, over a 1.5' x 1.5' region around the IRAS position. We also observed the high density tracers CS and HCO+ toward the source. The cold dust distribution was analyzed using submillimeter continuum data at 870 \mu\ obtained with the APEX telescope. Complementary IR and radio data at different wavelengths were used to complete the study of the ISM. The molecular gas distribution reveals a cavity and a shell-like structure of ~ 0.32 pc in radius centered at the position of the IRAS source, with some young stellar objects (YSOs) projected onto the cavity. The total molecular mass in the shell and the mean H$_2$ volume density are ~ 40 solar masses and ~(1-2) x 10$^3$ cm$^{-3}$, respectively. The cold dust counterpart of the molecular shell has been detected in the far-IR at 870 \mu\ and in Herschel data at 350 \mu. Weak extended emission at 24 \mu\ from warm dust is projected onto the cavity, as well as weak radio continuum emission. A comparison of the distribution of cold and warm dust, and molecular and ionized gas allows us to conclude that a compact HII region has developed in the molecular clump, indicating that this is an area of recent massive star formation. Probable exciting sources capable of creating the compact HII region are investigated. The 2MASS source 10380461-5846233 (MSX G286.3773-00.2563) seems to be responsible for the formation of the HII region., Comment: Accepted in A&A. 11 pages, 10 Postscript figures
Published: 2014
Full Text: View/download PDF

36. Molecules, dust, and protostars in NGC 3503

Author: Duronea, N. U., Vasquez, J., Romero, G. A., Cappa, C. E., Barbá, R., and Bronfman, L.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We are presenting here a follow-up study of the molecular gas and dust in the environs of the star forming region NGC 3503. This study aims at dealing with the interaction of NGC 3503 with its parental molecular cloud, and also with the star formation in the region. To analyze the molecular gas we use CO(2-1), 13CO(2-1), C18O(2-1), and HCN(3-2) line data obtained with the APEX telescope. To study the distribution of the dust, we make use of images at 870 microns from the ATLASGAL survey and IRAC-GLIMPSE archival images. We use public 2MASS and WISE data to search for candidate YSOs in the region. The new APEX observations allowed the substructure of the molecular gas in the velocity range from -28 to -23 km/s to be imaged in detail. The morphology of the molecular gas close to the nebula, the location of the PDR, and the shape of radio continuum emission suggest that the ionized gas is expanding against its parental cloud, and confirm the "champagne flow" scenario. We have identified several molecular clumps and determined some of their physical and dynamical properties. We have compared the physical properties of the clumps to investigate how the molecular gas has been affected by the HII region. Clumps adjacent to the ionization fronts of NGC 3503 and/or the bright rimmed cloud SFO62 have been heated and compressed by the ionized gas, but their line width is not different to those that are too distant to the ionization fronts. We identified several candidate YSOs in the region. Their spatial distribution suggests that stellar formation might have been boosted by the expansion of the nebula. We discard the "collect and collapse" scenario and propose alternative mechanisms such as radiatively driven implosion on pre-existing molecular clumps or small-scale Jeans gravitational instabilities., Comment: 18 pages, 13 figures. Accepted for publication in A&A
Published: 2014
Full Text: View/download PDF

37. THE NUMBER OF EXTRANODAL SITES IN NODAL PTCL: A PROPOSAL FOR A FEASIBLE PROGNOSTIC MARKER FOR OUTCOMES IN LOW-INCOME COUNTRIES. A COLLABORATIVE STUDY GRUPO DE ESTUDIO LATINO-AMERICANO DE LINFOPROLIFERATIVO (GELL) & T-CELL BRAZIL PROJECT (TCBP)

Author: Fischer, T, Miranda, E, Pereira, J, Duffles, G, Tavares, JV, Castro, NS, Silva, RSA, Farias, DLC, Brasil, SAB, Macedo, CCG, Colaço, C, Baptista, RLR, Cecyn, KZ, Bortucchi, D, Barros, GFS, Nabhan, S, Radtke, PPG, Schaffel, R, Zing, N, Nogueira, FL, Cunha-Junior, AD, Clé, DV, Filho, JTDS, Figueiredo, VLP, Pont, MD, Gaiolla, R, Hamerschlak, N, Ribeiro, EFO, Hallack-Neto, A, Dias, MA, Gonzaga, Y, Rabelo, YS, Teixeira, L, Perini, G, Conhalato, MALHM, Cury, P, Idrobo, H, Castro, D, Beltran, B, Enriquez, D, Vasquez, J, Roche, C, Artiles, D, Valvert, F, Villela, L, Oliver, C, Korin, L, Pena, C, Roa, M, Viera, MAT, Gasenapp, AV, Quiroz, A, Figari, CS, Rios, R, Paredes, S, Saul, EE, Bermack, C, Meza, K, Valcarcel, B, Souza, CA, Malpica, L, and Chiattone, CS
Published: 2024
Full Text: View/download PDF

38. Analysis of a multistage solar thermal energy accumulator

Author: Reyes, A., Pailahueque, N., Henríquez-Vargas, L., Vásquez, J., and Sepúlveda, F.
Published: 2019
Full Text: View/download PDF

39. Review of the main colour vision clinical assessment tests

Author: Fanlo Zarazaga, A., Gutiérrez Vásquez, J., and Pueyo Royo, V.
Published: 2019
Full Text: View/download PDF

40. Revisión de los principales test clínicos para evaluar la visión del color

Author: Fanlo Zarazaga, A., Gutiérrez Vásquez, J., and Pueyo Royo, V.
Published: 2019
Full Text: View/download PDF

41. Measurement of the Mass Difference Between Top and Anti-top Quarks at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: We present a measurement of the mass difference between top ($t$) and anti-top ($\bar{t}$) quarks using $t\bar{t}$ candidate events reconstructed in the final state with one lepton and multiple jets. We use the full data set of Tevatron $\sqrt{s} = 1.96$ TeV proton-antiproton collisions recorded by the CDF II detector, corresponding to an integrated luminosity of 8.7 fb$^{-1}$. We estimate event-by-event the mass difference to construct templates for top-quark signal events and background events. The resulting mass difference distribution of data compared to signal and background templates using a likelihood fit yields $\Delta M_{top} = {M}_{t} - {M}_{\bar{t}} = -1.95 $pm$ 1.11 (stat) $pm$ 0.59 (syst)$ and is in agreement with the standard model prediction of no mass difference., Comment: Accepted in Phys. Rev. D
Published: 2012
Full Text: View/download PDF

42. Search for the Higgs boson in the all-hadronic final state using the full CDF data set

Author: CDF Collaboration, Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: This paper reports the result of a search for the standard model Higgs boson in events containing four reconstructed jets associated with quarks. For masses below 135GeV/c2, Higgs boson decays to bottom-antibottom quark pairs are dominant and result primarily in two hadronic jets. An additional two jets can be produced in the hadronic decay of a W or Z boson produced in association with the Higgs boson, or from the incoming quarks that produced the Higgs boson through the vector-boson fusion process. The search is performed using a sample of \sqrt{s} = 1.96 TeV proton-antiproton collisions corresponding to an integrated luminosity of 9.45 fb-1 recorded by the CDF II detector. The data are in agreement with the background model and 95% credibility level upper limits on Higgs boson production are set as a function of the Higgs boson mass. The median expected (observed) limit for a 125GeV/c2 Higgs boson is 11.0 (9.0) times the predicted standard model rate., Comment: Submitted to Journal of High Energy Physics
Published: 2012
Full Text: View/download PDF

43. Precision Top-Quark Mass Measurements at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: We present a precision measurement of the top-quark mass using the full sample of Tevatron $\sqrt{s}=1.96$ TeV proton-antiproton collisions collected by the CDF II detector, corresponding to an integrated luminosity of 8.7 $fb^{-1}$. Using a sample of $t\bar{t}$ candidate events decaying into the lepton+jets channel, we obtain distributions of the top-quark masses and the invariant mass of two jets from the $W$ boson decays from data. We then compare these distributions to templates derived from signal and background samples to extract the top-quark mass and the energy scale of the calorimeter jets with {\it in situ} calibration. The likelihood fit of the templates from signal and background events to the data yields the single most-precise measurement of the top-quark mass, $\mtop = 172.85 $\pm$ 0.71 (stat) $\pm$ 0.85 (syst) GeV/c^{2}.$, Comment: submitted to Phys. Rev. Lett
Published: 2012
Full Text: View/download PDF

44. An inclusive search for the Higgs boson in the four-lepton final state at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: An inclusive search for the standard model Higgs boson using the four-lepton final state in proton-antiproton collisions produced by the Tevatron at sqrt(s) = 1.96 TeV is conducted. The data are recorded by the CDF II detector and correspond to an integrated luminosity of 9.7 /fb. Three distinct Higgs decay modes, namely ZZ, WW, and tau-tau, are simultaneously probed. Nine potential signal events are selected and found to be consistent with the background expectation. We set a 95% credibility limit on the production cross section times the branching ratio and subsequent decay to the four lepton final state for hypothetical Higgs boson masses between 120 GeV/c^2 and 300 GeV/c^2., Comment: 8 pages, 3 figures
Published: 2012
Full Text: View/download PDF

45. Molecular gas towards G18.8+1.8

Author: Vasquez, J., Rubio, M., Cappa, C. E., and Duronea, N. U.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: This work aims at investigating the characteristics of the molecular gas associated with the nebula G18.8+1.8, linked to the Wolf-Rayet star HD168206 (WR 113), and its relation to other components of its local interstellar medium. We carried out molecular observations of the 12CO(J=1-0) and (J=2-1) lines with angular resolution of 44 arcsec and 22 arcsec using the SEST telescope. Complementary NANTEN data of the 12CO(1-0) line were also used. The dust emission was analyzed using Spitzer-IRAC images at 8.0 microns, and WISE data at 3.4, 4.6, and 12.0 microns. The SEST data allowed us to identify a molecular component (Cloud 3) having velocities in the interval from ~ +30 to +36 km/s which is most probably linked to the nebula. Morphological and kinematical properties suggest that Cloud 3 constitute a wind-blown molecular half-shell, which expands around WR113. The ratio R_(2-1/1-0) and excitation temperatures indicate that the molecular gas is being irradiated by strong UV radiation. The location of the inner optical ring in the outer edge of Cloud 3 suggests that the stars SerOB2-1, -2, -3, -63, and -64 are responsables for the ionization of Cloud 3 and the inner ring nebula. A comparison between the spatial distribution of the molecular gas and the PAH emission at 8 $\mu$m indicates the existence of a PDR between the ionized and the molecular gas. A search for candidate young stellar objects (YSOs) in the region around G18.8+1.8 based on available 2MASS, MSX, IRAS, and Spitzer-IRAC catalogs resulted in the detection of about sixty sources, some of them projected onto Cloud 3. Two small spots of clustered candidates YSOs are projected near the outer border of Cloud 3, although a triggered stellar formation scenario is doubtful., Comment: 12 pages, 9 figures, accepted for publication in A&A
Published: 2012
Full Text: View/download PDF

46. Measurement of ZZ production in leptonic final states at {\surd}s of 1.96 TeV at CDF

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: In this paper we present a precise measurement of the total ZZ production cross section in pp collisions at {\surd}s= 1.96 TeV, using data collected with the CDF II detector corresponding to an integrated luminosity of approximately 6 fb-1. The result is obtained by combining separate measurements in the four-charged (lll'l'), and two-charged-lepton and two-neutral-lepton (llvv) decay modes of the Z. The combined measured cross section for pp {\to} ZZ is 1.64^(+0.44)_(-0.38) pb. This is the most precise measurement of the ZZ production cross section in 1.96 TeV pp collisions to date., Comment: submitted to Phys. Rev. Lett
Published: 2011
Full Text: View/download PDF

47. Gibbs distribution analysis of temporal correlations structure in retina ganglion cells

Author: Vasquez, J. C., Marre, O., Palacios, A. G., Berry II, M. J., and Cessac, B.
Subjects: Quantitative Biology - Neurons and Cognition, Physics - Biological Physics
Abstract: We present a method to estimate Gibbs distributions with \textit{spatio-temporal} constraints on spike trains statistics. We apply this method to spike trains recorded from ganglion cells of the salamander retina, in response to natural movies. Our analysis, restricted to a few neurons, performs more accurately than pairwise synchronization models (Ising) or the 1-time step Markov models (\cite{marre-boustani-etal:09}) to describe the statistics of spatio-temporal spike patterns and emphasizes the role of higher order spatio-temporal interactions., Comment: To appear in J. Physiol. Paris
Published: 2011
Full Text: View/download PDF

48. Search for new phenomena in events with two $Z$ bosons and missing transverse momentum in $p\bar{p}$ collisions at $\sqrt{s}=1.96$ TeV

Author: Aaltonen, T., Gonzalez, B. Alvarez, Amerio, S., Amidei, D., Anastassov, A., Annovi, A., Antos, J., Apollinari, G., Appel, J. A., Apresyan, A., Arisawa, T., Artikov, A., Asaadi, J., Ashmanskas, W., Auerbach, B., Aurisano, A., Azfar, F., Badgett, W., Barbaro-Galtieri, A., Barnes, V. E., Barnett, B. A., Barria, P., Bartos, P., Bauce, M., Bauer, G., Bedeschi, F., Beecher, D., Behari, S., Bellettini, G., Bellinger, J., Benjamin, D., Beretvas, A., Bhatti, A., Binkley, M., Bisello, D., Bizjak, I., Bland, K. R., Blumenfeld, B., Bocci, A., Bodek, A., Bortoletto, D., Boudreau, J., Boveia, A., Brigliadori, L., Brisuda, A., Bromberg, C., Brucken, E., Bucciantonio, M., Budagov, J., Budd, H. S., Budd, S., Burkett, K., Busetto, G., Bussey, P., Buzatu, A., Calancha, C., Camarda, S., Campanelli, M., Campbell, M., Canelli, F., Carls, B., Carlsmith, D., Carosi, R., Carrillo, S., Carron, S., Casal, B., Casarsa, M., Castro, A., Catastini, P., Cauz, D., Cavaliere, V., Cavalli-Sforza, M., Cerri, A., Cerrito, L., Chen, Y. C., Chertok, M., Chiarelli, G., Chlachidze, G., Chlebana, F., Cho, K., Chokheli, D., Chou, J. P., Chung, W. H., Chung, Y. S., Ciobanu, C. I., Ciocci, M. A., Clark, A., Clarke, C., Compostella, G., Convery, M. E., Conway, J., Corbo, M., Cordelli, M., Cox, C. A., Cox, D. J., Crescioli, F., Almenar, C. Cuenca, Cuevas, J., Culbertson, R., Dagenhart, D., d'Ascenzo, N., Datta, M., de Barbaro, P., De Cecco, S., De Lorenzo, G., Dell'Orso, M., Deluca, C., Demortier, L., Deng, J., Deninno, M., Devoto, F., d'Errico, M., Di Canto, A., Di Ruzza, B., Dittmann, J. R., D'Onofrio, M., Donati, S., Dong, P., Dorigo, M., Dorigo, T., Ebina, K., Elagin, A., Eppig, A., Erbacher, R., Errede, D., Errede, S., Ershaidat, N., Eusebi, R., Fang, H. C., Farrington, S., Feindt, M., Fernandez, J. P., Ferrazza, C., Field, R., Flanagan, G., Forrest, R., Frank, M. J., Franklin, M., Freeman, J. C., Funakoshi, Y., Furic, I., Gallinaro, M., Galyardt, J., Garcia, J. E., Garfinkel, A. F., Garosi, P., Gerberich, H., Gerchtein, E., Giagu, S., Giakoumopoulou, V., Giannetti, P., Gibson, K., Ginsburg, C. M., Giokaris, N., Giromini, P., Giunta, M., Giurgiu, G., Glagolev, V., Glenzinski, D., Gold, M., Goldin, D., Goldschmidt, N., Golossanov, A., Gomez, G., Gomez-Ceballos, G., Goncharov, M., Gonzalez, O., Gorelov, I., Goshaw, A. T., Goulianos, K., Grinstein, S., Grosso-Pilcher, C., Group, R. C., da Costa, J. Guimaraes, Gunay-Unalan, Z., Haber, C., Hahn, S. R., Halkiadakis, E., Hamaguchi, A., Han, J. Y., Happacher, F., Hara, K., Hare, D., Hare, M., Harr, R. F., Hatakeyama, K., Hays, C., Heck, M., Heinrich, J., Herndon, M., Hewamanage, S., Hidas, D., Hocker, A., Hopkins, W., Horn, D., Hou, S., Hughes, R. E., Hurwitz, M., Husemann, U., Hussain, N., Hussein, M., Huston, J., Introzzi, G., Iori, M., Ivanov, A., James, E., Jang, D., Jayatilaka, B., Jeon, E. J., Jha, M. K., Jindariani, S., Johnson, W., Jones, M., Joo, K. K., Jun, S. Y., Junk, T. R., Kamon, T., Karchin, P. E., Kasmi, A., Kato, Y., Ketchum, W., Keung, J., Khotilovich, V., Kilminster, B., Kim, D. H., Kim, H. S., Kim, H. W., Kim, J. E., Kim, M. J., Kim, S. B., Kim, S. H., Kim, Y. K., Kimura, N., Kirby, M., Klimenko, S., Kondo, K., Kong, D. J., Konigsberg, J., Kotwal, A. V., Kreps, M., Kroll, J., Krop, D., Krumnack, N., Kruse, M., Krutelyov, V., Kuhr, T., Kurata, M., Kwang, S., Laasanen, A. T., Lami, S., Lammel, S., Lancaster, M., Lander, R. L., Lannon, K., Lath, A., Latino, G., LeCompte, T., Lee, E., Lee, H. S., Lee, J. S., Lee, S. W., Leo, S., Leone, S., Lewis, J. D., Limosani, A., Lin, C. -J., Linacre, J., Lindgren, M., Lipeles, E., Lister, A., Litvintsev, D. O., Liu, C., Liu, Q., Liu, T., Lockwitz, S., Loginov, A., Lucchesi, D., Lueck, J., Lujan, P., Lukens, P., Lungu, G., Lys, J., Lysak, R., Madrak, R., Maeshima, K., Makhoul, K., Malik, S., Manca, G., Manousakis-Katsikakis, A., Margaroli, F., Marino, C., Martinez, M., Martinez-Ballarin, R., Mastrandrea, P., Mattson, M. E., Mazzanti, P., McFarland, K. S., McIntyre, P., McNulty, R., Mehta, A., Mehtala, P., Menzione, A., Mesropian, C., Miao, T., Mietlicki, D., Mitra, A., Miyake, H., Moed, S., Moggi, N., Mondragon, M. N., Moon, C. S., Moore, R., Morello, M. J., Morlock, J., Fernandez, P. Movilla, Mukherjee, A., Muller, Th., Murat, P., Mussini, M., Nachtman, J., Nagai, Y., Naganoma, J., Nakano, I., Napier, A., Nett, J., Neu, C., Neubauer, M. S., Nielsen, J., Nodulman, L., Norniella, O., Nurse, E., Oakes, L., Oh, S. H., Oh, Y. D., Oksuzian, I., Okusawa, T., Orava, R., Ortolan, L., Griso, S. Pagan, Pagliarone, C., Palencia, E., Papadimitriou, V., Paramonov, A. A., Patrick, J., Pauletta, G., Paulini, M., Paus, C., Pellett, D. E., Penzo, A., Phillips, T. J., Piacentino, G., Pianori, E., Pilot, J., Pitts, K., Plager, C., Pondrom, L., Poprocki, S., Potamianos, K., Poukhov, O., Prokoshin, F., Pronko, A., Ptohos, F., Pueschel, E., Punzi, G., Pursley, J., Rahaman, A., Ramakrishnan, V., Ranjan, N., Ray, J., Redondo, I., Renton, P., Rescigno, M., Riddick, T., Rimondi, F., Ristori, L., Robson, A., Rodrigo, T., Rodriguez, T., Rogers, E., Rolli, S., Roser, R., Rossi, M., Rubbo, F., Ruffini, F., Ruiz, A., Russ, J., Rusu, V., Safonov, A., Sakumoto, W. K., Sakurai, Y., Santi, L., Sartori, L., Sato, K., Saveliev, V., Savoy-Navarro, A., Schlabach, P., Schmidt, A., Schmidt, E. E., Schmidt, M. P., Schmitt, M., Schwarz, T., Scodellaro, L., Scribano, A., Scuri, F., Sedov, A., Seidel, S., Seiya, Y., Semenov, A., Sforza, F., Sfyrla, A., Shalhout, S. Z., Shears, T., Shepard, P. F., Shimojima, M., Shiraishi, S., Shochet, M., Shreyber, I., Simonenko, A., Sinervo, P., Sissakian, A., Sliwa, K., Smith, J. R., Snider, F. D., Soha, A., Somalwar, S., Sorin, V., Squillacioti, P., Stancari, M., Stanitzki, M., Denis, R. St., Stelzer, B., Stelzer-Chilton, O., Stentz, D., Strologas, J., Strycker, G. L., Sudo, Y., Sukhanov, A., Suslov, I., Takemasa, K., Takeuchi, Y., Tang, J., Tecchio, M., Teng, P. K., Thom, J., Thome, J., Thompson, G. A., Thomson, E., Ttito-Guzman, P., Tkaczyk, S., Toback, D., Tokar, S., Tollefson, K., Tomura, T., Tonelli, D., Torre, S., Torretta, D., Totaro, P., Trovato, M., Tu, Y., Ukegawa, F., Uozumi, S., Varganov, A., Vasquez, J., Vazquez, F., Velev, G., Vellidis, C., Vidal, M., Vila, I., Vilar, R., Vizan, J., Vogel, M., Volpi, G., Wagner, P., Wagner, R. L., Wakisaka, T., Wallny, R., Wang, S. M., Warburton, A., Waters, D., Weinberger, M., Wester III, W. C., Whitehouse, B., Whiteson, D., Wicklund, A. B., Wicklund, E., Wilbur, S., Wick, F., Williams, H. H., Wilson, J. S., Wilson, P., Winer, B. L., Wittich, P., Wolbers, S., Wolfe, H., Wright, T., Wu, X., Wu, Z., Yamamoto, K., Yamaoka, J., Yang, T., Yang, U. K., Yang, Y. C., Yao, W. -M., Yeh, G. P., Yi, K., Yoh, J., Yorita, K., Yoshida, T., Yu, G. B., Yu, I., Yu, S. S., Yun, J. C., Zanetti, A., Zeng, Y., and Zucchelli, S.
Subjects: High Energy Physics - Experiment
Abstract: We present a search for new phenomena in events with two reconstructed $Z$ bosons and large missing transverse momentum, sensitive to processes $p\bar{p}\rightarrow X_2X_2 \rightarrow Z Z X_1 X_1$, where $X_2$ is an unstable particle decaying as $X_2\rightarrow ZX_1$ and $X_1$ is undetected. The particles $X_1$ and $X_2$ may be, among other possibilities, fourth generation neutrinos or supersymmetric particles. We study the final state in which one $Z$ boson decays to two charged leptons and the second decays hadronically. In data corresponding to an integrated luminosity of 4.2 fb$^{-1}$ from proton-antiproton collisions recorded by the CDF II detector at the Tevatron, with center-of-mass energy of 1.96 TeV, we find agreement between data and standard-model backgrounds. We calculate 95% confidence level upper limits on the cross section of the process $p\bar{p}\rightarrow X_2X_2 \rightarrow Z Z X_1 X_1$ ranging from 50 fb to 1 pb, depending on the masses of $X_1$ and $X_2$., Comment: 7 pages, 4 figures. Submitted Phys. Rev. D
Published: 2011
Full Text: View/download PDF

49. NGC 3503 and its molecular environment

Author: Duronea, N. U., Vasquez, J., Cappa, C. E., Corti, M., and Arnal, E. M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a study of the molecular gas and interstellar dust distribution in the environs of the HII region NGC 3503 associated with the open cluster Pis 17 with the aim of investigating the spatial distribution of the molecular gas linked to the nebula and achieving a better understanding of the interaction of the nebula and Pis 17 with their molecular environment. We based our study in ^{12}CO(1-0) observations of a region of ~0.6 deg. in size obtained with the 4-m NANTEN telescope, unpublished radio continuum data at 4800 and 8640 MHz obtained with the ATCA telescope, radio continuum data at 843 MHz obtained from SUMSS, and available IRAS, MSX, IRAC-GLIMPSE, and MIPSGAL images. We found a molecular cloud (Component 1) having a mean velocity of -24.7 km s^{-1}, compatible with the velocity of the ionized gas, which is associated with the nebula and its surroundings. Adopting a distance of 2.9 +/- 0.4 kpc the total molecular mass and density yield (7.6 +/- 2.1) x 10^3 Msun and 400 +/- 240 cm^{-3}, respectively. The radio continuum data confirm the existence of an electron density gradient in NGC 3503. The IR emission shows the presence of a PDR bordering the higher density regions of the nebula. The spatial distribution of the CO emission shows that the nebula coincides with a molecular clump, with the strongest CO emission peak located close to the higher electron density region. The more negative velocities of the molecular gas (about -27 km s^{-1}), is coincident with NGC 3503. Candidate YSOs were detected towards the HII region, suggesting that embedded star formation may be occurring in the neighbourhood of the nebula. The presence of a clear electron density gradient, along with the spatial distribution of the molecular gas and PAHs in the region indicates that NGC 3503 is a blister-type HII region that probably has undergone a champagne phase.
Published: 2011
Full Text: View/download PDF

50. A multifrequency study of the active star forming complex NGC6357. I. Interstellar structures linked to the open cluster Pis24

Author: Cappa, C. E., Barbá, R., Duronea, N. U., Vasquez, J., Arnal, E. M., Goss, W. M., and Lajús, E. Fernández
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We investigate the distribution of the gas (ionized, neutral atomic and molecular), and interstellar dust in the complex star forming region NGC6357 with the goal of studying the interplay between the massive stars in the open cluster Pis24 and the surrounding interstellar matter. Our study of the distribution of the ionized gas is based on narrow-band Hhalfa, [SII], and [OIII] images obtained with the Curtis-Schmidt Camera at CTIO, Chile, and on radio continuum observations at 1465 MHz taken with the VLA with a synthesized beam of 40 arcsec. The distribution of the molecular gas is analyzed using 12CO(1-0) data obtained with the Nanten radiotelescope, Chile (angular resolution = 2.7 arcmin). The interstellar dust distribution was studied using mid-infrared data from the GLIMPSE survey and far-infrared observations from IRAS. NGC6357 consists of a large ionized shell and a number of smaller optical nebulosities. The optical, radio continuum, and near- and mid-IR images delineate the distributions of the ionized gas and interstellar dust in the HII regions and in previously unknown wind blown bubbles linked to the massive stars in Pis24 revealing surrounding photodissociation regions. The CO line observations allowed us to identify the molecular counterparts of the ionized structures in the complex and to confirm the presence of photodissociation regions. The action of the WR star HD157504 on the surrounding gas was also investigated. The molecular mass in the complex is estimated to be (4+/-2)X10^5 Mo. Mean electron densities derived from the radio data suggest electron densities > 200 cm^-3, indicating that NGC6357 is a complex formed in a region of high ambient density. The known massive stars in Pis24 and a number of newly inferred massive stars are mainly responsible for the excitation and photodissociation of the parental molecular cloud., Comment: 16 pages, 9 figures. Accepted for publication in MNRAS
Published: 2011
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Region

Database

Publisher

658 results on '"Vásquez, J."'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources