Philip A Pinto

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Scholarly Contributions

Books

• {Pinto}, P. (1988). The late-time spectra of supernovae.

Journals/Publications

• Salcedo, A. N., Wibking, B. D., Weinberg, D. H., Wu, H., Ferrer, D., Eisenstein, D., & Pinto, P. (2020). Cosmology with stacked cluster weak lensing and cluster-galaxy cross-correlations. mnras, 491(3), 3061-3081.
• Garrison, L. H., Eisenstein, D. J., & Pinto, P. A. (2019). A high-fidelity realization of the Euclid code comparison N-body simulation with ABACUS. mnras, 485(3), 3370-3377.
• Wibking, B. D., Salcedo, A. N., Weinberg, D. H., Garrison, L. H., Ferrer, D., Tinker, J., Eisenstein, D., Metchnik, M., & Pinto, P. (2019). Emulating galaxy clustering and galaxy-galaxy lensing into the deeply non-linear regime: methodology, information, and forecasts. mnras, 484(1), 989-1006.
• {Wang}, X., {Wang}, L., {Filippenko}, A., {Baron}, E., {Kromer}, M., {Jack}, D., {Zhang}, T., {Aldering}, G., {Antilogus}, P., {Arnett}, W., {Baade}, D., {Barris}, B., {Benetti}, S., {Bouchet}, P., {Burrows}, A., {Canal}, R., {Cappellaro}, E., {Carlberg}, R., {di Carlo}, E., , {Challis}, P., et al. (2012). Evidence for Type Ia Supernova Diversity from Ultraviolet Observations with the Hubble Space Telescope. Astrophysical Journal, 749, 126.
• Mehta, K. T., Seo, H., Eckel, J., Eisenstein, D. J., Metchnik, M., Pinto, P., & Xiaoying, X. u. (2011). Galaxy bias and its effects on the baryon acoustic oscillation measurements. Astrophysical Journal, 734(2).
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  Abstract: The baryon acoustic oscillation (BAO) feature in the clustering of matter in the universe serves as a robust standard ruler and hence can be used to map the expansion history of the universe. We use high force resolution simulations to analyze the effects of galaxy bias on the measurements of the BAO signal. We apply a variety of Halo Occupation Distributions (HODs) and produce biased mass tracers to mimic different galaxy populations. We investigate whether galaxy bias changes the nonlinear shifts on the acoustic scale relative to the underlying dark matter distribution presented by Seo etal. For the less biased HOD models (b < 3), we do not detect any shift in the acoustic scale relative to the no-bias case, typically 0.10% ± 0.10%. However, the most biased HOD models (b > 3) show a shift at moderate significance (0.79% ± 0.31% for the most extreme case). We test the one-step reconstruction technique introduced by Eisenstein etal. in the case of realistic galaxy bias and shot noise. The reconstruction scheme increases the correlation between the initial and final (z = 1) density fields, achieving an equivalent level of correlation at nearly twice the wavenumber after reconstruction. Reconstruction reduces the shifts and errors on the shifts. We find that after reconstruction the shifts from the galaxy cases and the dark matter case are consistent with each other and with no shift. The 1σ systematic errors on the distance measurements inferred from our BAO measurements with various HODs after reconstruction are about 0.07%-0.15%. © 2011. The American Astronomical Society. All rights reserved.
• {Mehta}, K., {Seo}, H., {Eckel}, J., {Eisenstein}, D., {Metchnik}, M., {Pinto}, P., , X. (2011). Galaxy Bias and Its Effects on the Baryon Acoustic Oscillation Measurements. Astrophysical Journal, 734, 94.
• Ridgway, S., Cook, K., Miller, M., Petry, C., Chandrasekharan, S., Saha, A., Allsman, R., Axelrod, T., Claver, C., Delgado, F., Ivezic, Z., Jones, R. L., Krughoff, S., Pierfederici, F., & Pinto, P. (2010). Simulation of autonomous observing with a ground-based telescope: The LSST experience. Proceedings of SPIE - The International Society for Optical Engineering, 7737.
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  Abstract: A survey program with multiple science goals will be driven by multiple technical requirements. On a ground-based telescope, the variability of conditions introduces yet greater complexity. For a program that must be largely autonomous with minimal dwell time for efficiency it may be quite difficult to foresee the achievable performance. Furthermore, scheduling will likely involve self-referential constraints and appropriate optimization tools may not be available. The LSST project faces these issues, and has designed and implemented an approach to performance analysis in its Operations Simulator and associated post-processing packages. The Simulator has allowed the project to present detailed performance predictions with a strong basis from the engineering design and measured site conditions. At present, the Simulator is in regular use for engineering studies and science evaluation, and planning is underway for evolution to an operations scheduling tool. We will describe the LSST experience, emphasizing the objectives, the accomplishments and the lessons learned. © 2010 Copyright SPIE - The International Society for Optical Engineering.
• Seo, H., Eckel, J., Eisenstein, D. J., Mehta, K., Metchnik, M., Padmanabhan, N., Pinto, P., Takahashi, R., White, M., & Xiaoying, X. u. (2010). High-precision predictions for the acoustic scale in the nonlinear regime. Astrophysical Journal Letters, 720(2), 1650-1667.
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  Abstract: We measure shifts of the acoustic scale due to nonlinear growth and redshift distortions to a high precision using a very large volume of high-force-resolution simulations. We compare results from various sets of simulations that differ in their force, volume, and mass resolution. We find a consistency within 1.5s for shift values from different simulations and derive shift α(z) - 1 = (0.300 ± 0.015) %[D(z)/D(0)]2 using our fiducial set. We find a strong correlation with a non-unity slope between shifts in real space and in redshift space and a weak correlation between the initial redshift and low redshift. Density-field reconstruction not only removes the mean shifts and reduces errors on the mean, but also tightens the correlations. After reconstruction, we recover a slope of near unity for the correlation between the real and redshift space and restore a strong correlation between the initial and the low redshifts. We derive propagators and mode-coupling terms from our N-body simulations and compare with the Zel'dovich approximation and the shifts measured from the χ2 fitting, respectively. We interpret the propagator and the mode-coupling term of a nonlinear density field in the context of an average and a dispersion of its complex Fourier coefficients relative to those of the linear density field; from these two terms, we derive a signal-to-noise ratio of the acoustic peak measurement. We attempt to improve our reconstruction method by implementing 2LPT and iterative operations, but we obtain little improvement. The Fisher matrix estimates of uncertainty in the acoustic scale is tested using 5000 h-3 Gpc3 of cosmological Particle-Mesh simulations from Takahashi et al. At an expected sample variance level of 1%, the agreement between the Fisher matrix estimates based on Seo and Eisenstein and the N-body results is better than 10%. © 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A.
• Xu, X., White, M., Padmanabhan, N., Eisenstein, D. J., Eckel, J., Mehta, K., Metchnik, M., Pinto, P., & Seo, H. -. (2010). A new statistic for analyzing baryon acoustic oscillations. Astrophysical Journal Letters, 718(2), 1224-1234.
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  Abstract: We introduce a new statistic ωℓ(rs ) for measuring and analyzing large-scale structure and particularly the baryon acoustic oscillations. ωℓ(rs ) is a band-filtered, configuration space statistic that is easily implemented and has advantages over the traditional power spectrum and correlation function estimators. Unlike these estimators, ωℓ(rs ) can localize most of the acoustic information into a single dip at the acoustic scale while avoiding sensitivity to the poorly constrained large-scale power (i.e., the integral constraint) through the use of a localized and compensated filter. It is also sensitive to anisotropic clustering through pair counting and does not require any binning of data.We measure the shift in the acoustic peak due to nonlinear effects using the monopole ω0(rs ) derived from subsampled dark matter (DM) catalogs as well as from mock galaxy catalogs created via halo occupation distribution modeling. All of these are drawn from 44 realizations of 10243 particle DM simulations in a 1 h -1 Gpc box at z = 1. We compare these shifts with those obtained from the power spectrum and conclude that the results agree.We therefore expect that distance measurements obtained from ω0(rs ) and P(k) will be consistent with each other.We also show that it is possible to extract the same amount of acoustic information by fitting over a finite range using either ω0(rs ) or P(k) derived from equal volume surveys. © 2010. The American Astronomical Society. All rights reserved.
• {Xu}, X., {White}, M., {Padmanabhan}, N., {Eisenstein}, D., {Eckel}, J., {Mehta}, K., {Metchnik}, M., {Pinto}, P., , H. (2010). A New Statistic for Analyzing Baryon Acoustic Oscillations. Astrophysical Journal, 718, 1224-1234.
• Collaboration}, {. S., {Abell}, P., {Allison}, J., {Anderson}, S., {Andrew}, J., {Angel}, J., {Armus}, L., {Arnett}, D., {Asztalos}, S., {Axelrod}, T., & al., e. (2009). LSST Science Book, Version 2.0. ArXiv e-prints.
• Ivezic}, Z., {Axelrod}, T., {Brandt}, W., {Burke}, D., {Claver}, C., {Connolly}, A., {Cook}, K., {Gee}, P., {Gilmore}, D., {Jacoby}, S., {Jones}, R., {Kahn}, S., {Kantor}, J., {Krabbendam}, V., {Lupton}, R., {Monet}, D., {Pinto}, P., {Saha}, A., {Schalk}, T., , {Schneider}, D., et al. (2008). Large Synoptic Survey Telescope: From Science Drivers To Reference Design. Serbian Astronomical Journal, 176, 1-13.
• Ivezić, Ž., Axelrod, T., Becker, A. C., Becla, J., Borne, K., Burke, D. L., Claver, C. F., Cook, K. H., Connolly, A., Gilmore, D. K., Jones, R. L., Jurić, M., Kahn, S. M., Lim, K. -., Lupton, R. H., Monet, D. G., Pinto, P. A., Sesar, B., Stubbs, C. W., & Tyson, J. A. (2008). Parametrization and classification of 20 billion LSST objects: Lessons from SDSS. AIP Conference Proceedings, 1082, 359-365.
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  Abstract: The Large Synoptic Survey Telescope (LSST) will be a large, wide-field ground-based system designed to obtain, starting in 2015, multiple images of the sky that is visible from Cerro Pachon in Northern Chile. About 90% of the observing time will be devoted to a deep-wide-fast survey mode which will observe a 20,000 deg 2 region about 1000 times during the anticipated 10 years of operations (distributed over six bands, ugrizy). Each 30-second long visit will deliver 5σ depth for point sources of r ∼ 24.5 on average. The co-added map will be about 3 magnitudes deeper, and will include 10 billion galaxies and a similar number of stars. We discuss various measurements that will be automatically performed for these 20 billion sources, and how they can be used for classification and determination of source physical and other properties. We provide a few classification examples based on SDSS data, such as color classification of stars, color-spatial proximity search for wide-angle binary stars, orbital-color classification of asteroid families, and the recognition of main Galaxy components based on the distribution of stars in the position-metallicity-kinematics space. Guided by these examples, we anticipate that two grand classification challenges for LSST will be 1) rapid and robust classification of sources detected in difference images, and 2) simultaneous treatment of diverse astrometric and photometric time series measurements for an unprecedentedly large number of objects. © 2008 .American Institute of Physics.
• Ivezić, Ž., Axelrod, T., Brandt, W. N., Burke, D. L., Claver, C. F., Connolly, A., Cook, K. H., Gee, P., Gilmore, D. K., Jacoby, S. H., Jones, R. L., Kahn, S. M., Kantor, J. P., Krabbendam, V., Lupton, R. H., Monet, D. G., Pinto, P. A., Saha, A., Schalk, T. L., , Schneider, D. P., et al. (2008). Large synoptic survey telescope: From science drivers to reference design. Serbian Astronomical Journal, 1-13.
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  Abstract: In the history of astronomy, major advances in our understanding of the Universe have come from dramatic improvements in our ability to accurately measure astronomical quantities. Aided by rapid progress in information technology, current sky surveys are changing the way we view and study the Universe. Next-generation surveys will maintain this revolutionary progress. We focus here on the most ambitious survey currently planned in the visible band, the Large Synoptic Survey Telescope (LSST). LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: constraining dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. It will be a large, wide-field ground-based system designed to obtain multiple images covering the sky that is visible from Cerro Pachón in Northern Chile. The current baseline design, with an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg2 field of view, and a 3,200 Megapixel camera, will allow about 10,000 square degrees of sky to be covered using pairs of 15-second exposures in two photometric bands every three nights on average. The system is designed to yield high image quality, as well as superb astrometric and photometric accuracy. The survey area will include 30,000 deg2 with δ < +34.5°, and will be imaged multiple times in six bands, ugrizy, covering the wavelength range 320-1050 nm. About 90% of the observing time will be devoted to a deep-wide-fast survey mode which will observe a 20,000 deg2 region about 1000 times in the six bands during the anticipated 10 years of operation. These data will result in databases including 10 billion galaxies and a similar number of stars, and will serve the majority of science programs. The remaining 10% of the observing time will be allocated to special programs such as Very Deep and Very Fast time domain surveys. We describe how the LSST science drivers led to these choices of system parameters.
• Zhan, H., Wang, L., Pinto, P., & Tyson, J. A. (2008). Measuring baryon acoustic oscillations with millions of supernovae. Astrophysical Journal, 675(1 PART 2), L1-L4.
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  Abstract: Since Type Ia supernovae (SNe) explode in galaxies, they can, in principle, be used as the same tracer of the large-scale structure as their hosts to measure baryon acoustic oscillations (BAOs). To realize this, one must obtain a dense integrated sampling of SNe over a large fraction of the sky, which may only be achievable photometrically with future projects such as the Large Synoptic Survey Telescope. The advantage of SN BAOs is that SNe have more uniform luminosities and more accurate photometric redshifts than galaxies, but the disadvantage is that they are transitory and hard to obtain in large number at high redshift. We find that a half-sky photometric SN survey to redshift z = 0.8 is able to measure the baryon signature in the SN spatial power spectrum. Although dark energy constraints from SN BAOs are weak, they can significantly improve the results from SN luminosity distances of the same data, and the combination of the two is no longer sensitive to cosmic microwave background priors. © 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A.
• {Ivezic}, Z., {Tyson}, J., {Abel}, B., {Acosta}, E., {Allsman}, R., {AlSayyad}, Y., {Anderson}, S., {Andrew}, J., {Angel}, R., {Angeli}, G., {Ansari}, R., {Antilogus}, P., {Arndt}, K., {Astier}, P., {Aubourg}, E., {Axelrod}, T., {Bard}, D., {Barr}, J., {Barrau}, A., , {Bartlett}, J., et al. (2008). LSST: from Science Drivers to Reference Design and Anticipated Data Products. ArXiv e-prints.
• {Zhan}, H., {Wang}, L., {Pinto}, P., , J. (2008). Measuring Baryon Acoustic Oscillations with Millions of Supernovae. Astrophysical Journal Letters, 675, L1.
• Ivezić, Ž., Monet, D. G., Bond, N., Jurić, M., Sesar, B., Munn, J. A., Lupton, R. H., Gunn, J. E., Knapp, G. R., Tyson, A. J., Pinto, P., & Cook, K. (2007). Astrometry with digital sky surveys: From SDSS to LSST. Proceedings of the International Astronomical Union, 3(S248), 537-543.
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  Abstract: Major advances in our understanding of the Universe have historically come from dramatic improvements in our ability to accurately measure astronomical quantities. The astrometric observations obtained by modern digital sky surveys are enabling unprecedentedly massive and robust studies of the kinematics of the Milky Way. For example, the astrometric data from the Sloan Digital Sky Survey (SDSS), together with half a century old astrometry from the Palomar Observatory Sky Survey (POSS), have enabled the construction of a catalog that includes absolute proper motions as accurate as 3 mas/year for about 20 million stars brighter than V=20, and for 80,000 spectroscopically confirmed quasars which provide exquisite error assessment. We discuss here several ongoing studies of Milky Way kinematics based on this catalog. The upcoming next-generation surveys will maintain this revolutionary progress. For example, we show using realistic simulations that the Large Synoptic Survey Telescope (LSST) will measure proper motions accurate to 1 mas/year to a limit 4 magnitude fainter than possible with SDSS and POSS catalogs, or with the Gaia survey. LSST will also obtain geometric parallaxes with accuracy similar to Gaia's at its faint end (0.3 mas at V=20), and extend them to V=24 with an accuracy of 3 mas. We discuss the impact that these LSST measurements will have on studies of the Milky Way kinematics, and potential synergies with the Gaia survey. © 2008 Copyright International Astronomical Union.
• Hamuy, M., Folatelli, G., Morrell, N. I., Phillips, M. M., Suntzeff, N. B., Persson, S. E., Roth, M., Gonzalez, S., Krzeminski, W., Contreras, C., Freedman, W. L., Murphy, D. C., Madore, B. F., Wyatt, P., Maza, J., Filippenko, A. V., Weidong, L. I., & Pinto, P. A. (2006). The Carnegie Supernova Project: The low-redshift survey. Publications of the Astronomical Society of the Pacific, 118(839), 2-20.
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  Abstract: Supernovae are essential to understanding the chemical evolution of the universe. Type la supernovae also provide the most powerful observational tool currently available for studying the expansion history of the universe and the nature of dark energy. Our basic knowledge of supernovae comes from the study of their photometric and spectroscopic properties. However, the presently available data sets of optical and nearinfrared light curves of supernovae are rather small and/or heterogeneous, and employ photometric systems that are poorly characterized. Similarly, there are relatively few supernovae whose spectral evolution has been well sampled, both in wavelength and phase, with precise spectrophotometric observations. The low-redshift portion of the Carnegie Supernova Project (CSP) seeks to remedy this situation by providing photometry and spectrophotometry of a large sample of supernovae taken on telescope/filter/detector systems that are well understood and well characterized. During a 5 year program that began in 2004 September, we expect to obtain high-precision u'g'r'i'BVYJHK s light curves and optical spectrophotometry for about 250 supernovae of all types. In this paper we provide a detailed description of the CSP survey observing and data reduction methodology. In addition, we present preliminary photometry and spectra obtained for a few representative supernovae during the first observing campaign. © 2006. The Astronomical Society of the Pacific. All rights reserved.
• Yang, Y., Zabludoff, A. I., Davé, R., Eisenstein, D. J., Pinto, P. A., Katz, N., Weinberg, D. H., & Barton, E. J. (2006). Probing galaxy formation with He II cooling lines. Astrophysical Journal Letters, 640(2 I), 539-552.
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  Abstract: Using high-resolution cosmological simulations, we study hydrogen and helium gravitational cooling radiation from gas accretion by young galaxies. We focus on the He II cooling lines, which arise from gas with a different temperature history (Tmax ∼ 105 K) than H I line-emitting gas. We examine whether three major atomic cooling lines, H I λ1216, He II λ1640, and He II λ304, are observable, finding that Lyα and He II λ1640 cooling emission at z = 2-3 are potentially detectable with deep narrowband (R > 100) imaging and/or spectroscopy from the ground. While the expected strength of H I λ1216 cooling emission depends strongly on the treatment of the self-shielded phase of the IGM in the simulations, our predictions for the He II 11640 line are more robust, because the He II emissivity is negligible below T ∼ 10 4.5 K and less sensitive to the UV background. Although He II λ1640 cooling emission is fainter than Lyα by at least a factor of 10 and, unlike Lyα, might not be resolved spatially with current observational facilities, it is more suitable to study gas accretion in the galaxy formation process because it is optically thin and less contaminated by the recombination lines from star-forming galaxies. The He II λ1640 line can be used to distinguish among mechanisms for powering the so-called Lyα blobs - including gravitational cooling radiation, photoionization by stellar populations, and starburst-driven superwinds - because (1) He II λ1640 emission is limited to very low metallicity [log (Z/Z⊙) ≲-5.3] and Population III stars and (2) the blob's kinematics are probed unambiguously through the He II line width, which for cooling radiation is narrower (σ < 400 km s-1) than typical wind speeds. © 2006. The American Astronomical Society, All rights reserved.
• {Hamuy}, M., {Folatelli}, G., {Morrell}, N., {Phillips}, M., {Suntzeff}, N., {Persson}, S., {Roth}, M., {Gonzalez}, S., {Krzeminski}, W., {Contreras}, C., {Freedman}, W., {Murphy}, D., {Madore}, B., {Wyatt}, P., {Maza}, J., {Filippenko}, A., {Li}, W., , P. (2006). The Carnegie Supernova Project: The Low-Redshift Survey. Publications Astronomical Society of the Pacific, 118, 2-20.
• {Yang}, Y., {Zabludoff}, A., {Dav{\'e}}, R., {Eisenstein}, D., {Pinto}, P., {Katz}, N., {Weinberg}, D., , E. (2006). Probing Galaxy Formation with He II Cooling Lines. Astrophysical Journal, 640, 539-552.
• Krisciunas, K., Suntzeff, N. B., Phillips, M. M., Candia, P., Prieto, J. L., Antezana, R., Chassagne, R., Chen, H., Dickinson, M., Eisenhardt, P. R., Espinoza, J., Garnavich, P. M., Gonzalez, D., Harrison, T. E., Hamuy, M., Ivanov, V. D., Krzemiński, W., Kulesa, C., McCarthy, P., , Moro-Martin, A., et al. (2005). Erratum: Optical and infrared photometry of the type Ia supernovae 1991T, 1991bg, 1999ek, 2001bt, 2001cn, 2001cz, and 2002bo (Astronomical Journal (2004) 128 (3034)). Astronomical Journal, 130(1), 350-.
• MacRossan, M. N., Metchnik, M. V., & Pinto, P. A. (2005). Hypersonic flow over a wedge with a particle flux method. AIP Conference Proceedings, 762, 650-655.
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  Abstract: We have investigated the use of DSMC as a pseudo-Euler solver in the continuum limit by using a modification of Pullin's Equilibrium Particle Simulation Method (EPSM). EPSM is a particle-based method which is in effect the large collision rate limit of DSMC yet requires far less computational effort. We propose a modification of EPSM, the Particle Flux Method (PFM), which is intermediate between EPSM and a conventional finite volume continuum flow solver. The total mass, momentum and energy in each cell are stored. Flux particles are created at every time step and move in free flight over a short decoupling time step, carrying mass momentum and energy between cells. The new method has been demonstrated by calculating the hypersonic flow over a wedge, for which DSMC calculations are available. Because of an inherent dissipation, related to the cell size and time step, the shock was thicker than that found in the DSMC calculations, but the shock location was the same. PFM is not prohibitively expensive and may have some advantages over conventional continuum based flow solvers, in terms of robustness arising from its firm basis in the physics of molecular flow. © 2005 American Institute of Physics.
• {Krisciunas}, K., {Suntzeff}, N., {Phillips}, M., {Candia}, P., {Prieto}, J., {Antezana}, R., {Chassagne}, R., {Chen}, H., {Dickinson}, M., {Eisenhardt}, P., {Espinoza}, J., {Garnavich}, P., {Gonzalez}, D., {Harrison}, T., {Hamuy}, M., {Ivanov}, V., {Krzemi{\'n}ski}, W., {Kulesa}, C., {McCarthy}, P., , {Moro-Martin}, A., et al. (2005). Erratum: ``Optical and Infrared Photometry of the Type Ia Supernovae 1991T, 1991bg, 1999ek, 2001bt, 2001cn, 2001cz, and 2002bo'' (AJ, 128, 3034 [2004]). Astronomical Journal, 130, 350-350.
• Claver, C. F., Sweeney, D., Tyson, J. A., Althouse, B., Axelrod, T., Cook, K., Daggert, L., Kantor, J., Kahn, S., Krabbendam, V. L., Pinto, P., Sebag, J., Stubbs, C., & Wolff, S. C. (2004). Project status of the 8.4m LSST. Proceedings of SPIE - The International Society for Optical Engineering, 5489(PART 2), 705-716.
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  Abstract: The 8.4m Large Synoptic Survey Telescope (LSST) is a wide-field telescope facility that will add a qualitatively new capability in astronomy. For the first time, the LSST will provide time-lapse digital imaging of faint astronomical objects across the entire sky. The LSST has been identified as a national scientific priority by diverse national panels, including multiple National Academy of Sciences committees. This judgment is based upon the LSST's ability to address some of the most pressing open questions in astronomy and fundamental physics, while driving advances in data-intensive science and computing. The LSST will provide unprecedented 3-dimensional maps of the mass distribution in the Universe, in addition to the traditional images of luminous stars and galaxies. These mass maps can be used to better understand the nature of the newly discovered and utterly mysterious Dark Energy that is driving the accelerating expansion of the Universe. The LSST will also provide a comprehensive census of our solar system, including potentially hazardous asteroids as small as 100 meters in size. The LSST facility consists of three major subsystems: 1) the telescope, 2) the camera and 3) the data processing system. The baseline design for the LSST telescope is a 8.4m 3-mirror design with a 3.5 degree field of view resulting in an A-Omega product (etendue) of 302deg 2m 2. The camera consists of 3-element transmisive corrector producing a 64cm diameter flat focal plane. This focal plane will be populated with roughly 3 billion 10μm pixels. The data processing system will include pipelines to monitor and assess the data quality, detect and classify transient events, and establish a large searchable object database. We report on the status of the designs for these three major LSST subsystems along with the overall project structure and management.
• Hawreliak, J., Chambers, D. M., Glenzer, S. H., Gouveia, A., Kingham, R. J., Marjoribanks, R. S., Pinto, P. A., Renner, O., Soundhauss, P., Topping, S., Wolfrum, E., Young, P. E., & Wark, J. S. (2004). Thomson scattering measurements of heat flow in a laser-produced plasma. Journal of Physics B: Atomic, Molecular and Optical Physics, 37(7), 1541-1551.
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  Abstract: Measurements of the electron distribution and heat flow between the critical and ablation surfaces in a laser-produced plasma have been obtained using Thomson scattering. A frequency-quadrupled probe beam was used to obtain Thomson spectra at above-critical densities in a plasma produced by irradiation of solid targets with the fundamental laser light at irradiances of 3 × 1014 W cm-2. Comparison of Thomson spectra at the ion acoustic frequency (sensitive to the cold return current) with simulated spectra shows that the data are consistent with Fokker-Planck simulations of the electron distribution function, providing the first direct information on the electron distribution function.
• Hawreliak, J., Chambers, {. M., Glenzer, {. H., Gouveia, A., Kingham, {. J., Marjoribanks, {. S., Pinto, {. A., Renner, O., Soundhauss, P., Topping, S., Wolfrum, E., Young, {. E., & Wark, {. S. (2004). Thomson scattering measurements of heat flow in a laser-produced plasma. Journal of Physics B: Atomic, Molecular and Optical Physics, 37, 1541--1551.
• Krisciunas, K., Suntzeff, N. B., Phillips, M. M., Candia, P., Prieto, J. L., Antezana, R., Chassagne, R., Chen, H., Dickinson, M., Eisenhardt, P. R., Espinoza, J., Garnavich, P. M., González, D., Harrison, T. E., Hamuy, M., Ivanov, V. D., Krzemiński, W., Kulesa, C., McCarthy, P., , Moro-Martín, A., et al. (2004). Optical and infrared photometry of the type Ia supernovae 1991T, 1991bg, 1999ek, 2001bt, 2001cn, 2001cz, and 2002bo. Astronomical Journal, 128(6), 3034-3052.
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  Abstract: We present optical and/or infrared photometry of the Type la supernovae SN 1991T, SN 1991bg, SN 1999ek, SN 2001bt, SN 2001cn, SN 2001cz, and SN 2002bo. All but one of these supernovae have decline rate parameters, Δm 15(B), close to the median value of 1.1 for the whole class of Type la supernovae. The addition of these supernovae to the relationship between the near-infrared absolute magnitudes and Δm 15(B) strengthens the previous relationships we have found in that the maximum light absolute magnitudes are essentially independent of the decline rate parameter. (SN 1991bg, the prototype of the subclass of fast-declining Type Ia supernovae, is a special case.) The dispersion in the Hubble diagram in JHK is only ∼0.15 mag. The near-infrared properties of Type Ia supernovae continue to be excellent measures of the luminosity distances to the supernova host galaxies because of the need for only small corrections from the epoch of observation to maximum light, low dispersion in absolute magnitudes at maximum light, and the minimal reddening effects in the near-infrared.
• Milne, P. A., Hungerford, A. L., Fryer, C. L., Evans, T. M., Urbatsch, T. J., Boggs, S. E., Isern, J., Bravo, E., Hirschmann, A., Kumagai, S., Pinto, P. A., & The, L. -. (2004). Unified one-dimensional simulations of gamma-ray line emission from Type Ia supernovae. Astrophysical Journal Letters, 613(2 I), 1101-1119.
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  Abstract: The light curves of Type Ia supernovac (SNe Ia) are powered by gamma rays emitted by the decay of radioactive elements such as 56Ni and its decay products. These gamma rays are downscattered, absorbed, and eventually reprocessed into the optical emission that makes up the bulk of all SN observations. Detection of the gamma rays that escape the expanding star provide the only direct means to study this power source for SN Ia light curves. Unfortunately, disagreements between calculations for the gamma-ray lines have made it difficult to interpret any gamma-ray observations. Here we present a detailed comparison of the major gamma-ray line transport codes for a series of one-dimensional SN Ia models. Discrepancies in past results were due to errors in the codes, and the corrected versions of the seven different codes yield very similar results. This convergence of the simulation results allows us to infer more reliable information from the current set of gamma-ray observations of SNe Ia. The observations of SN 1986G, SN 1991T, and SN 1998bu are consistent with explosion models based on their classification: subluminous, superluminous, and normally luminous, respectively.
• {Krisciunas}, K., {Suntzeff}, N., {Phillips}, M., {Candia}, P., {Prieto}, J., {Antezana}, R., {Chassagne}, R., {Chen}, H., {Dickinson}, M., {Eisenhardt}, P., {Espinoza}, J., {Garnavich}, P., {Gonz{\'a}lez}, D., {Harrison}, T., {Hamuy}, M., {Ivanov}, V., {Krzemi{\'n}ski}, W., {Kulesa}, C., {McCarthy}, P., , {Moro-Mart{\'{\i}}n}, A., et al. (2004). Optical and Infrared Photometry of the Type Ia Supernovae 1991T, 1991bg, 1999ek, 2001bt, 2001cn, 2001cz, and 2002bo. Astronomical Journal, 128, 3034-3052.
• {Milne}, P., {Hungerford}, A., {Fryer}, C., {Evans}, T., {Urbatsch}, T., {Boggs}, S., {Isern}, J., {Bravo}, E., {Hirschmann}, A., {Kumagai}, S., {Pinto}, P., , L. (2004). Unified One-Dimensional Simulations of Gamma-Ray Line Emission from Type Ia Supernovae. Astrophysical Journal, 613, 1101-1119.
• Gouveia, A., Al'miev, I., Hawreliak, J., Chambers, D. M., Liang, T., Marjoribanks, R., Pinto, P. A., Renner, O., Zhang, J., & Wark, J. S. (2003). Absorption spectroscopy of Al XIII Ly-α radiation by an Fe XXIV plasma. Journal of Quantitative Spectroscopy and Radiative Transfer, 81(1-4), 199-207.
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  Abstract: We report an analysis of absorption and fluorescence spectroscopy of the interaction of Al XIII Ly- radiation with Fe XXIV in laser-produced plasmas. These results were obtained in the context of exploring a Al-Fe photopumped X-ray laser scheme. Aluminium/iron targets were used in different geometries in order to observe in detail the transition mechanisms of the Al/Fe photopumping scheme. The absorption of the Al XIII Ly- emission by the Fe XXIV plasma was observed after traversing different lengths of an Fe plasma. A simple radiation transfer model is being developed as a post-processor to the 1-D hydro-code MED103 in order to simulate these results. We also report some experimental evidence that may indicate that enhanced fluorescence of Fe XXIV 5d-2p transition could have occurred due to photopumping by the Al radiation despite any direct evidence of photopumped XUV lasing. © 2003 Elsevier Science Ltd. All rights reserved.
• Gouveia, A., Al'miev, {. R., Hawreliak, J., Chambers, {. M., Liang, T., Marjoribanks, R., Pinto, {. A., Renner, O., Zhang, J., & Wark, {. S. (2003). Absorption spectroscopy of Al XIII Ly-α radiation by an Fe XXIV plasma. Journal of Quantitative Spectroscopy and Radiative Transfer, 81, 199--207.
• Thompson, T. A., Burrows, A., & Pinto, P. A. (2003). Shock breakout in core-collapse supernovae and its neutrino signature. Astrophysical Journal Letters, 592(1 I), 434-456.
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  Abstract: We present results from dynamical models of core-collapse Supernovae in one spatial dimension, employing a newly developed Boltzmann neutrino radiation transport algorithm, coupled to Newtonian Lagrangian hydrodynamics and a consistent high-density nuclear equation of state. The transport method is multigroup, employs the Feautrier technique, uses the tangent-ray approach to resolve angles, is implicit in time, and is second-order accurate in space. We focus on shock breakout and follow the dynamical evolution of the cores of 11, 15, and 20 M⊙ progenitors through collapse and the first 250 ms after bounce. The shock breakout burst is the signal event in core-collapse evolution, is the brightest phenomenon in astrophysics, and is largely responsible for the initial debilitation and stagnation of the bounce shock. As such, its detection and characterization could test fundamental aspects of the current collapse/supernova paradigm. We examine the effects on the emergent neutrino spectra, light curves, and mix of species (particularly in the early postbounce epoch) of artificial opacity changes, the number of energy groups, the weak magnetism/recoil corrections, nucleon-nucleon bremsstrahlung, neutrino-electron scattering, and the compressibility of nuclear matter. Furthermore, we present the first high-resolution look at the angular distribution of the neutrino radiation field both in the semitransparent regime and at large radii and explore the accuracy with which our tangent-ray method tracks the free propagation of a pulse of radiation in a near vacuum. Finally, we fold the emergent neutrino spectra with the efficiencies and detection processes for a selection of modern underground neutrino observatories and argue that the prompt electron-neutrino breakout burst from the next galactic supernova is in principle observable and usefully diagnostic of fundamental collapse/supernova behavior. Although we are not in this study focusing on the supernova mechanism per se, our simulations support the theoretical conclusion (already reached by others) that spherical (one-dimensional) supernovae do not explode when good physics and transport methods are employed.
• {Thompson}, T., {Burrows}, A., , P. (2003). Shock Breakout in Core-Collapse Supernovae and Its Neutrino Signature. Astrophysical Journal, 592, 434-456.
• Chambers, D. M., Pinto, P. A., Hawreliak, J., Al'Miev, I. R., Gouveia, A., Sondhauss, P., Wolfrum, E., Wark, J. S., Glenzer, S. H., Lee, R. W., Young, P. E., Renner, O., Marjoribanks, R. S., & Topping, S. (2002). \textit{K} -shell spectroscopy of an independently diagnosed uniaxially expanding laser-produced aluminum plasma. Phys. Rev. E, 66, 026410.
• Chambers, D. M., Pinto, P. A., Hawreliak, J., Al'Miev, I., Gouveia, A., Sondhauss, P., Wolfrum, E., Wark, J. S., Glenzer, S. H., Lee, R. W., Young, P. E., Renner, O., Marjoribanks, R. S., & Topping, S. (2002). K-shell spectroscopy of an independently diagnosed uniaxially expanding laser-produced aluminum plasma. Physical Review E - Statistical, Nonlinear, and Soft Matter Physics, 66(2), 026410/1-026410/16.
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  Abstract: We present detailed spectroscopic analysis of the primary K-shell emission lines from a uniaxially expanding laser-produced hydrogenic and heliumlike aluminum plasma. The spectroscopic measurements are found to be consistent with time-dependent hydrodynamic properties of the plasma, measured using Thomson scattering and shadowgraphy. The K-shell population kinetics code FLY with the measured hydrodynamic parameters is used to generate spectra that are compared to the experimental spectra. Excellent agreement is found between the measured and calculated spectra for a variety of experimental target widths employed to produce plasmas with different optical depths. The peak emission from the hydrogenic Lyman series is determined to be from a temporal and spatial region where the hydrodynamic parameters are essentially constant. This allows a single steady-state solution of FLY to be used to deduce the electron temperature and density, from the measured line ratios and linewidths, for comparison with the Thomson and shadowgraphy data. These measurements are found to agree well with time-dependent calculations, and provide further validation for the FLY calculations of the ionization and excitation balance for a K-shell aluminum plasma. We also discuss the possible application of this data as a benchmark for hydrodynamic simulations and ionization/excitation balance calculations. © 2002 The American Physical Society.
• Hamuy, M., & Pinto, P. A. (2002). Type II supernovae as standardized candles. Astrophysical Journal Letters, 566(2 II), L63-L65.
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  Abstract: We present evidence for a correlation between expansion velocities of the ejecta of Type II plateau supernovae and their bolometric luminosities during the plateau phase. This correlation permits one to standardize the candles and decrease the scatter in the Hubble diagram from ∼1 mag to levels of 0.4 and 0.3 mag in the V and I bands, respectively. When we restrict the sample to the eight objects that are well in the Hubble flow (cz > 3000 km s-1), the scatter drops even further, to only 0.2 mag (or 9% in distance), which is comparable to the precision yielded by Type la supernovae and is far better than the "expanding photosphere method" applied to Type II Supernovae. Using SN 1987A to calibrate the Hubble diagrams, we get H0 = 55 ± 12.
• Hamuy, M., Maza, J., Pinto, P. A., Phillips, M. M., Suntzeff, N. B., Blum, R. D., Olsen, K. A., Pinfield, D. J., Ivanov, V. D., Augusteijn, T., Brillant, S., Chadid, M., Cuby, J. -., Doublier, V., Hainaut, O. R., Floc'h, E. L., Lidman, C., Petr-Gotzens, M. G., Pompei, E., & Vanzi, L. (2002). Erratum: Optical and infrared spectroscopy of SN 1999ee and SN 1999ex (Astronomical Journal (2002) 124 (417)). Astronomical Journal, 124(4 1762), 2339-2340.
• Hamuy, M., Maza, J., Pinto, P. A., Phillips, M. M., Suntzeff, N. B., Blum, R. D., Olsen, K. A., Pinfield, D. J., Ivanov, V. D., Augusteijn, T., Brillant, S., Chadid, M., Cuby, J. -., Doublier, V., Hainaut, O. R., Floc'h, E. L., Lidman, C., Petr-Gotzens, M. G., Pompei, E., & Vanzi, L. (2002). Optical and infrared spectroscopy of SN 1999ee and SN 1999ex. Astronomical Journal, 124(1 1759), 417-429.
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  Abstract: We report optical and infrared spectroscopic observations of the Type Ia SN 1999ee and the Type Ib/c SN 1999ex, both of which were hosted by the galaxy IC 5179. For SN 1999ee we obtained a continuous sequence with an unprecedented wavelength and temporal coverage beginning 9 days before maximum light and extending through day 42. Before maximum light SN 1999ee displayed a normal spectrum with a strong Si II λ6355 absorption, thus showing that not all slow-declining supernovae (SNe) are spectroscopically peculiar at these evolutionary phases. A comparative study of the infrared spectra of SN 1999ee and other Type Ia SNe shows that there is a remarkable homogeneity among the Branch-normal SNe Ia during their first 60 days of evolution. SN 1991bg-like objects, on the other hand, display spectroscopic peculiarities at infrared wavelengths. SN 1999ex was characterized by the lack of hydrogen lines, weak optical He I lines, and strong He I λλ10830, 20581, thus providing an example of an intermediate case between pure Ib and Ic supernovae. We conclude, therefore, that SN 1999ex provides the first clear evidence for a link between the Ib and Ic classes and that there is a continuous spectroscopic sequence ranging from the He-deficient SNe Ic to the SNe Ib, which are characterized by strong optical He I lines.
• Harrison, F. A., Boggs, S. E., Christensen, F. E., Gehrels, N., Grindlay, J. E., Chen, C. M., Craig, W. W., Hailey, C. J., Pinto, P., Thorsett, S. E., Tueller, J., Windt, D., & Woosley, S. E. (2002). The High-Resolution Spectroscopic Imaging (HSI) Mission. Proceedings of SPIE - The International Society for Optical Engineering, 4851(1), 345-352.
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  Abstract: The High-Resolution Spectroscopic Imaging Mission is designed to be the first instrument to make true images of the hard X-ray/soft gamma-ray (2 - 600 keV) sky. By focusing energetic X-rays and low-energy gamma-rays, HSI will observe the cosmos with an unprecedented combination of sensitivity, spectral resolution, and angular resolving power. HSI is based on an array of multilayer grazing-incidence optics focusing onto high-resolution solid-state germanium pixel detectors with a focal length of 30 - 50 m. This paper describes the primary scientific objectives, technical approach to the instrumentation, and mission design.
• {Avelino}, P., {Martins}, C., , P. (2002). Modified Median Statistics and Type Ia Supernova Data. Astrophysical Journal, 575, 989-995.
• {Hamuy}, M., , P. (2002). Type II Supernovae as Standardized Candles. Astrophysical Journal Letters, 566, L63-L65.
• {Hamuy}, M., {Maza}, J., {Pinto}, P., {Phillips}, M., {Suntzeff}, N., {Blum}, R., {Olsen}, K., {Pinfield}, D., {Ivanov}, V., {Augusteijn}, T., {Brillant}, S., {Chadid}, M., {Cuby}, J., {Doublier}, V., {Hainaut}, O., {Le Floc'h}, E., {Lidman}, C., {Petr-Gotzens}, M., {Pompei}, E., , L. (2002). Erratum: ``Optical and Infrared Spectroscopy of SN 1999ee and SN 1999ex'' [Astron. J. 124, 417 (2002)]. Astronomical Journal, 124, 2339-2340.
• {Hamuy}, M., {Maza}, J., {Pinto}, P., {Phillips}, M., {Suntzeff}, N., {Blum}, R., {Olsen}, K., {Pinfield}, D., {Ivanov}, V., {Augusteijn}, T., {Brillant}, S., {Chadid}, M., {Cuby}, J., {Doublier}, V., {Hainaut}, O., {Le Floc'h}, E., {Lidman}, C., {Petr-Gotzens}, M., {Pompei}, E., , L. (2002). Optical and Infrared Spectroscopy of SN 1999ee and SN 1999ex. Astronomical Journal, 124, 417-429.
• Chambers, D. M., Glenzer, S. H., Hawreliak, J., Wolfrum, E., Gouveia, A., Lee, R. W., Marjoribanks, R. S., Renner, O., Sondhauss, P., Topping, S., Young, P. E., Pinto, P. A., & Wark, J. S. (2001). Detailed hydrodynamic and X-ray spectroscopic analysis of a laser-produced rapidly-expanding aluminium plasma. Journal of Quantitative Spectroscopy and Radiative Transfer, 71(2-6), 237-247.
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  Abstract: We present a detailed analysis of K-shell emission from laser-produced rapidly-expanding Al plasmas. This work forms part of a series of experiments performed at the Vulcan laser facility of the Rutherford Appleton Laboratory, UK. 1-D planar expansion was obtained by over-illuminating A1-microdot targets supported on CH plastic foils. The small size of the A1-plasma ensured high spatial and frequency resolution of the spectra, obtained with a single crystal spectrometer, two vertical dispersion variant double crystal spectrometers, and a vertical dispersion variant Johann Spectrometer. The hydrodynamic properties of the plasma were measured independently by spatially and temporally resolved Thomson scattering, utilizing a 4ω probe beam. This enabled sub- and super-critical densities to be probed relative to the 1ω heater beams. The deduced plasma hydrodynamic conditions are compared with those generated from the 1-D hydro-code Medusa, and the significant differences found in the electron temperature discussed. Synthetic spectra generated from the detailed term collisional radiative non-LTE atomic physics code Fly are compared with the experimental spectra for the measured hydrodynamic parameters, and for those taken from Medusa. Excellent agreement is only found for both the H- and He-like A1 series when careful account is taken of the temporal evolution of the electron temperature. © 2001 Published by Elsevier Science Ltd.
• Chambers, D., Glenzer, S., Hawreliak, J., Wolfrum, E., Gouveia, A., Lee, R., Marjoribanks, R., Renner, O., Sondhauss, P., Topping, S., Young, P., Pinto, P., & Wark, J. (2001). Detailed hydrodynamic and X-ray spectroscopic analysis of a laser-produced rapidly-expanding aluminium plasma. Journal of Quantitative Spectroscopy and Radiative Transfer, 71, 237 - 247.
• Hamuy, M., Pinto, P. A., Maza, J., Suntzeff, N. B., Phillips, M. M., Eastman, R. G., Smith, R. C., Corbally, C. J., Burstein, D., Yong, L. i., Ivanov, V., Moro-Martin, A., Strolger, L. G., Souza, R. D., Anjos, S. D., Green, E. M., Pickering, T. E., González, L., Antezana, R., , Wischnjewsky, M., et al. (2001). The distance to SN 1999em from the expanding photosphere method. Astrophysical Journal Letters, 558(2 PART 1), 615-642.
• Hawreliak, J., Chambers, D., Glenzer, S., Marjoribanks, R. S., Notley, M., Pinto, P., Renner, O., Sondhauss, P., Steel, R., Topping, S., Wolfrum, E., Young, P., & Wark, J. S. (2001). A Thomson scattering post-processor for the MEDUSA hydrocode. Journal of Quantitative Spectroscopy and Radiative Transfer, 71(2-6), 383-395.
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  Abstract: In order to understand the physical processes that occur in laser-produced plasmas it is necessary to diagnose the time-dependent hydrodynamic conditions. Thomson scattering is, in principle, an ideal diagnostic as it provides a non-intrusive method of measuring ion and electron temperature, electron density, plasma velocity, and heat flow. We describe here a post-processor for the MEDUSA hydrocode that simulates streak camera images of the Thomson spectra. The post-processor can be used in three ways: (1) creating simulated streak camera images that can be compared directly with experimental data, (2) evaluating experimental designs to determine the viability of the Thomson scattering diagnostic, and (3) as an automated data analysis routine for extracting hydrodynamic parameters from a calibrated experimental streak camera image. © 2001 Elsevier Science Ltd. All rights reserved.
• Pinto, P. A., & Eastman, R. G. (2001). The type Ia supernova width-luminosity relation. New Astronomy, 6(5), 307-319.
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  Abstract: Observations of type Ia supernovæ at high redshifts have become an important tool for studying the geometry of the universe. The relation between the duration of the peak phase of a type Ia supernova's lightcurve and its luminosity (broader is brighter) forms the cornerstone of this measurement, yet it is a purely empirical relation. In this paper we show that the relation is a natural consequence of the radiation transport in type Ia supernovae and suggest constraints on the nature of the explosions which arise from our interpretation of the observed relation. The principle parameter underlying the relation is the mass of radioactive 56Ni produced in the explosion. The relation is shown to be relatively insensitive to most other parameters in Chandrasekhar-mass explosions. Cosmological results are thus unlikely to suffer from systematic effects stemming from evolution in the explosions' progenitors.
• Pinto, P. A., Eastman, R. G., & Rogers, T. (2001). A test for the nature of the type ia supernova explosion mechanism. Astrophysical Journal Letters, 551(1 PART 1), 231-243.
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  Abstract: Currently, popular models for Type Ia supernovae (SNe Ia) fall into two general classes. The first comprises explosions of nearly pure carbon/oxygen (C/O) white dwarfs (WDs) at the Chandrasekhar limit which ignite near their centers. The second consists of lower mass C/O cores which are ignited by the detonation of an accreted surface helium layer. Explosions of the latter type produce copious Fe, Co, and Ni Kα emission from 56Ni and 56Co decay in the detonated surface layers, emission which is much weaker from Chandrasekhar-mass models. The presence of this emission provides a simple and unambiguous discriminant between these two models for SNe Ia. Both mechanisms may produce 0.1-0.6 M ⊙ of 56Ni, making them bright γ-ray line emitters. The time to maximum brightness of 56Ni decay lines is distinctly shorter in the M < M < Mch class of model (∼15 days) than in the Mch model (∼30 days), making γ-ray line evolution another direct test of the explosion mechanism. It should just be possible to detect K-shell emission from a sub-Mch explosion from SNe Ia as far away as the Virgo cluster with the XMM observatory. A 1-2 m2 X-ray telescope such as the proposed Constellation-X observatory could observe Kα emission from M < Mch SNe Ia in the Virgo cluster, providing not just a detection but high-accuracy flux and kinematic information.
• {Hamuy}, M., {Pinto}, P., {Maza}, J., {Suntzeff}, N., {Phillips}, M., {Eastman}, R., {Smith}, R., {Corbally}, C., {Burstein}, D., {Li}, Y., {Ivanov}, V., {Moro-Martin}, A., {Strolger}, L., {de Souza}, R., {dos Anjos}, S., {Green}, E., {Pickering}, T., {Gonz{\'a}lez}, L., {Antezana}, R., , {Wischnjewsky}, M., et al. (2001). The Distance to SN 1999em from the Expanding Photosphere Method. Astrophysical Journal, 558, 615-642.
• {Hamuy}, M., {Trager}, S., {Pinto}, P., {Phillips}, M., {Schommer}, R., {Ivanov}, V., , N. (2001). Erratum: ``A Search for Environmental Effects on Type Ia Supernovae'' [Astron. J. 120, 1479 (2000)]. Astronomical Journal, 122, 3506-3507.
• {Hubbard}, W., {Fortney}, J., {Lunine}, J., {Burrows}, A., {Sudarsky}, D., , P. (2001). Theory of Extrasolar Giant Planet Transits. Astrophysical Journal, 560, 413-419.
• {Pinto}, P., , R. (2001). The type Ia supernova width-luminosity relation. New Astronomy, 6, 307-319.
• {Pinto}, P., {Eastman}, R., , T. (2001). A Test for the Nature of the Type IA Supernova Explosion Mechanism. Astrophysical Journal, 551, 231-243.
• Burrows, A., Young, T., Pinto, P., Eastman, R., & Thompson, T. A. (2000). A new algorithm for supernova neutrino transport and some applications. Astrophysical Journal Letters, 539(2 PART 1), 865-887.
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  Abstract: We have developed an implicit, multigroup, time-dependent, spherical neutrino transport code based on the Feautrier variables, the tangent-ray method, and accelerated A iteration. The code achieves high angular resolution, is good to O(v/c), is equivalent to a Boltzmann solver (without gravitational redshifts), and solves the transport equation at all optical depths with precision. In this paper, we present our formulation of the relevant numerics and microphysics and explore protoneutron star atmospheres for snapshot postbounce models. Our major focus is on spectra, neutrino-matter heating rates, Eddington factors, angular distributions, and phase-space occupancies. In addition, we investigate the influence on neutrino spectra and heating of final-state electron blocking, stimulated absorption, velocity terms in the transport equation, neutrino-nucleon scattering asymmetry, and weak magnetism and recoil effects. Furthermore, we compare the emergent spectra and heating rates obtained using full transport with those obtained using representative flux-limited transport formulations to gauge their accuracy and viability. Finally, we derive useful formulae for the neutrino source strength due to nucleon-nucleon bremsstrahlung and determine bremsstrahlung's influence on the emergent vμ and vτ neutrino spectra. These studies are in preparation for new calculations of spherically symmetric core-collapse supernovae, proto neutron star winds, and neutrino signals.
• Hamuy, M., Trager, S. C., Pinto, P. A., Phillips, M. M., Schommer, R. A., Ivanov, V., & Suntzeff, N. B. (2000). A search for environmental effects on type Ia supernovae. Astronomical Journal, 120(3), 1479-1486.
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  Abstract: We use integrated colors and B and V absolute magnitudes of Type Ia supernova (SN) host galaxies in order to search for environmental effects on the SN optical properties. With the new sample of 44 SNe we confirm the conclusion by Hamuy et al. that bright events occur preferentially in young stellar environments. We find also that the brightest SNe occur in the least luminous galaxies, a possible indication that metal-poor neighborhoods produce the more luminous events. The interpretation of these results is made difficult, however, because of the fact that galaxies with younger stellar populations are also lower in luminosity. In an attempt to remove this ambiguity, we use models for the line strengths in the absorption spectrum of five early-type galaxies, in order to estimate metallicities and ages of the SN host galaxies. With the addition of abundance estimates from nebular analysis of the emission spectra of three spiral galaxies, we find possible further evidence that luminous SNe are produced in metal-poor neighborhoods. Further spectroscopic observations of the SN host galaxies will be necessary to test these results and assist in disentangling the age and metallicity effects on Type Ia SNe.
• Ivanov, V. D., Hamuy, M., & Pinto, P. A. (2000). On the relation between peak luminosity and parent population of type Ia supernovae: A new tool for probing the ages of distant galaxies. Astrophysical Journal Letters, 542(2 PART 1), 588-596.
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  Abstract: We study the properties of Type Ia supernovae (SNe Ia) as functions of the radial distance from their host galaxy centers. Using a sample of 62 SNe Ia with reliable luminosity, reddening, and decline rate determinations, we find no significant radial gradients of SNe Ia peak absolute magnitudes or decline rates in elliptical + S0 galaxies, suggesting that the diversity of SN properties is not related to the metallicity of their progenitors. We do find that the range in brightness and light curve width of supernovae in spiral galaxies extends to brighter, broader values. These results are interpreted as support for an age, but not metallicity, related origin of the diversity in SNe Ia. If confirmed with a larger and more accurate sample of data, the age-luminosity relation would offer a new and powerful tool to probe the ages and age gradients of stellar populations in galaxies at redshift as high as z ∼ 1-2. The absence of significant radial gradients in the peak (B-V)0 and (V-I)0 colors of SNe Ia supports the reddening correction method of Phillips et al. We find no radial gradient in residuals from the SN Ia luminosity-width relation, suggesting that the relation is not affected by properties of the progenitor populations and supporting the reliability of cosmological results based upon the use of SNe Ia as distance indicators.
• Pinto, P. A., & Eastman, R. G. (2000). The physics of Type Ia supernova light curves. I. Analytic results and time dependence. Astrophysical Journal Letters, 530(2 PART 1), 744-756.
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  Abstract: We develop an analytic solution of the radiation transport problem for Type Ia supernovae (SNe Ia) and show that it reproduces bolometric light curves produced by more detailed calculations under the assumption of a constant-extinction coefficient. This model is used to derive the thermal conditions in the interior of SNe Ia and to study the sensitivity of light curves to various properties of the underlying supernova explosions. Although the model is limited by simplifying assumptions, it is adequate for demonstrating that the relationship between SNe Ia maximum-light luminosity and rate of decline is most easily explained if SNe Ia span a range in mass. The analytic model is also used to examine the size of various terms in the transport equation under conditions appropriate to maximum light. For instance, the Eulerian and advective time derivatives are each shown to be of the same order of magnitude as other order v/c terms in the transport equation. We conclude that a fully time-dependent solution to the transport problem is needed in order to compute SNe Ia light curves and spectra accurate enough to distinguish subtle differences of various explosion models.
• Pinto, P. A., & Eastman, R. G. (2000). The physics of Type Ia supernova light curves. II. Opacity and diffusion. Astrophysical Journal Letters, 530(2 PART 1), 757-776.
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  Abstract: We examine the nature of the opacity and radiation transport in Type Ia supernovae. The dominant opacity arises from line transitions. We discuss the nature of line opacities and diffusion in expanding media and the appropriateness of various mean and expansion opacities used in light-curve calculations. Fluorescence is shown to be the dominant physical process governing the rate at which energy escapes the supernova. We present a sample light curve that was obtained using a time-dependent solution of the radiative transport equation with a spectral resolution of 80 km s-1 and employing an LTE equation of state. The result compares favorably with light curves and spectra of typical supernovae and is used to illustrate the physics controlling the evolution of the light curve and especially the secondary maxima seen in infrared photometry.
• Sudarsky, D., Burrows, A., & Pinto, P. (2000). Albedo and reflection spectra of extrasolar giant planets. Astrophysical Journal Letters, 538(2 PART 1), 885-903.
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  Abstract: We generate theoretical albedo and reflection spectra for a full range of extrasolar giant planet (EGP) models, from Jovian to 51 Pegasi class objects. Our albedo modeling utilizes the latest atomic and molecular cross sections, Mie theory treatment of scattering and absorption by condensates, a variety of particle size distributions, and an extension of the Feautrier technique, which allows for a general treatment of the scattering phase function. We find that, because of qualitative similarities in the compositions and spectra of objects within each of five broad effective temperature ranges, it is natural to establish five representative EGP albedo classes. At low effective temperatures (Teff ≲ 150 K) is a class of "Jovian" objects (class I) with tropospheric ammonia clouds. Somewhat warmer class II, or "water cloud," EGPs are primarily affected by condensed H2O. Gaseous methane absorption features are prevalent in both classes. In the absence of nonequilibrium condensates in the upper atmosphere, and with sufficient H2O condensation, class II objects are expected to have the highest visible albedos of any class. When the upper atmosphere of an EGP is too hot for H2O to condense, radiation generally penetrates more deeply. In these objects, designated class III or "clear" because of a lack of condensation in the upper atmosphere, absorption lines of the alkali metals, sodium and potassium, lower the albedo significantly throughout the visible. Furthermore, the near-infrared albedo is negligible, primarily because of strong CH4 and H2O molecular absorption and collision-induced absorption (CIA) by H2 molecules. In those EGPs with exceedingly small orbital distance ("roasters") and 900 K ≲ Teff ≲ 1500 K (class IV), a tropospheric silicate layer is expected to exist. In all but the hottest (Teff ≳ 1500 K) or lowest gravity roasters, the effect of this silicate layer is likely to be insignificant because of the very strong absorption by sodium and potassium atoms above the layer. The resonance lines of sodium and potassium are expected to be salient features in the reflection spectra of these EGPs. In the absence of nonequilibrium condensates, we find, in contrast to previous studies, that these class IV roasters likely have the lowest visible and Bond albedos of any class, rivaling the lowest albedos of our solar system. For the small fraction of roasters with Teff ≳ 1500 K and/or low surface gravity (≲103 cm s-2; class V), the silicate layer is located very high in the atmosphere, reflecting much of the incident radiation before it can reach the absorbing alkali metals and molecular species. Hence, the class V roasters have much higher albedos than those of class IV. In addition, for class V objects, UV irradiation may result in significant alkali metal ionization, thereby further weakening the alkali metal absorption lines. We derive Bond albedos (AB) and Teff estimates for the full set of known EGPs. A broad range in both values is found, with Teff ranging from ∼150 to nearly 1600 K, and AB from ∼0.02 to 0.8. We find that variations in particle size distributions and condensation fraction can have large quantitative, or even qualitative, effects on albedo spectra. In general, less condensation, larger particle sizes, and wider size distributions result in lower albedos. We explore the effects of nonequilibrium condensed products of photolysis above or within principal cloud decks. As in Jupiter, such species can lower the UV/blue albedo substantially, even if present in relatively small mixing ratios.
• {Burrows}, A., {Young}, T., {Pinto}, P., {Eastman}, R., , T. (2000). A New Algorithm for Supernova Neutrino Transport and Some Applications. Astrophysical Journal, 539, 865-887.
• {Hamuy}, M., {Trager}, S., {Pinto}, P., {Phillips}, M., {Schommer}, R., {Ivanov}, V., , N. (2000). A Search for Environmental Effects on Type IA Supernovae. Astronomical Journal, 120, 1479-1486.
• {Ivanov}, V., {Hamuy}, M., , P. (2000). On the Relation between Peak Luminosity and Parent Population of Type IA Supernovae: A New Tool for Probing the Ages of Distant Galaxies. Astrophysical Journal, 542, 588-596.
• {Pinto}, P., , R. (2000). The Physics of Type IA Supernova Light Curves. I. Analytic Results and Time Dependence. Astrophysical Journal, 530, 744-756.
• {Pinto}, P., , R. (2000). The Physics of Type IA Supernova Light Curves. II. Opacity and Diffusion. Astrophysical Journal, 530, 757-776.
• {Pinto}, P., , R. (2000). The Type Ia Supernova Width-Luminosity Relation. ArXiv Astrophysics e-prints.
• {Sudarsky}, D., {Burrows}, A., , P. (2000). Albedo and Reflection Spectra of Extrasolar Giant Planets. Astrophysical Journal, 538, 885-903.
• Fryer, C. L., Colgate, S. A., & Pinto, P. A. (1999). Iron opacity and the pulsar of SN 1987A. Astrophysical Journal Letters, 511(2 PART 1), 885-895.
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  Abstract: Neutron stars formed in Type II supernovae are likely to be initially obscured by late-time fallback. Although much of the late-time fallback is quickly accreted via neutrino cooling, some material remains on the neutron star, forming an atmosphere that slowly accretes through photon emission. In this paper, we derive structure equations of the fallback atmosphere and present results of one-dimensional simulations of that fallback. The atmosphere remaining after neutrino cooling (Lν) becomes unimportant (Lν ≲ LEdd,e-, the Compton Eddington limit) is only a fraction of the total mass accreted (≲ 10-8Macc = 10-9M⊙). Recombined iron dominates the opacity in the outer regions, leading to an opacity 103-104 times higher than that of electron scattering alone. The resultant photon emission of the remnant atmosphere is limited to ≲ 10-3LEdd,e-. The late-time evolution of this system leads to the formation of a photon-driven wind from the accretion of the inner portion of the atmosphere, leaving, for most cases, a bare neutron star on timescales shorter than 1 yr. The degenerate remnant of 1987A may not be a black hole. Instead, the fallback material may have already accreted or blown off in the accretion-driven wind. If the neutron star has either a low magnetic field or a low rotational spin frequency, we would not expect to see the neutron star remnant of 1987A.
• Hamuy, M., & Pinto, P. A. (1999). Selection effects, biases, and constraints in the Calán/Tololo supernova survey. Astronomical Journal, 117(3), 1185-1205.
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  Abstract: We use Monte Carlo simulations of the Calán/Tololo photographic supernova survey to show that a simple model of the survey's selection effects accounts for the observed distributions of recession velocity, apparent magnitude, angular offset, and projected radial distance between the supernova and the host galaxy nucleus for this sample of Type Ia supernovae (SNe Ia). The model includes biases due to the flux-limited nature of the survey, the different light-curve morphologies displayed by different SNe Ia, and the difficulty of finding events projected near the central regions of the host galaxies. From these simulations we estimate the bias in the zero point and slope of the absolute magnitude-decline rate relation used in SNe Ia distance measurements. For an assumed intrinsic scatter of 0.15 mag about this relation, these selection effects decrease the zero point by 0.04 mag. The slope of the relation is not significantly biased. We conclude that despite selection effects in the survey, the shape and zero point of the relation determined from the Calán/Tololo sample are quite reliable. We estimate the degree of incompleteness of the survey as a function of decline rate and estimate a corrected luminosity function for SNe Ia in which the frequency of SNe appears to increase with decline rate (the fainter SNe are more common). Finally, we compute the integrated detection efficiency of the survey in order to infer the rate of SNe Ia from the 31 events found. For a value of H0 = 65 km s-1 Mpc-1 we obtain a SN Ia rate of 0.21+0.30-0.13 SNu. This is in good agreement with the value 0.16 ± 0.05 SNe recently determined by Capellaro et al.
• Miller, D. L., & Pinto, P. (1999). Synthetic spectra and lightcurves of supernovae-the black hole of atomic physics needs. Physica Scripta T, 83, 125-127.
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  Abstract: The modeling of the radiation transport in supernova atmospheres is discussed in terms of lightcurve physics and spectral synthesis. The importance of accurate and complete atomic physics is discussed. The elements and ionization stages which are important for supernova calculations are listed as well as the processes for which data are required. © Physica Scripta 1999.
• {Fryer}, C., {Colgate}, S., , P. (1999). Iron Opacity and the Pulsar of SN 1987A. Astrophysical Journal, 511, 885-895.
• {Hamuy}, M., , P. (1999). Selection Effects, Biases, and Constraints in the Cal{\'A}n/Tololo Supernova Survey. Astronomical Journal, 117, 1185-1205.
• {Miller}, D., , P. (1999). Synthetic Spectra and Lightcurves of Supernovae - The Black Hole of Atomic Physics Needs. Physica Scripta Volume T, 83, 125-127.
• Bowers, E. J., Meikle, W. P., Geballe, T. R., Walton, N. A., Pinto, P. A., Dhillon, V. S., Howell, S. B., & Harrop-Allin, M. (1997). Infrared and optical spectroscopy of Type Ia supernovae in the nebular phase. Monthly Notices of the Royal Astronomical Society, 290(4), 663-679.
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  Abstract: We present near-infrared (NIR) spectra for Type la supernovae at epochs of 13 to 338 d after maximum blue light. Some contemporary optical spectra are also shown. All the NIR spectra exhibit considerable structure throughout the J, H and K bands. In particular, they exhibit a flux 'deficit' in the J band which persists as late as 175 d. This is responsible for the well-known red J-H colour. To identify the emission features and test the 56Ni hypothesis for the explosion and subsequent light curve, we compare the NIR and optical nebular-phase data with a simple non-LTE nebular spectral model. We find that many of the spectral features are due to iron-group elements, and that the J-band deficit is due to a lack of emission lines from species that dominate the rest of the IR/optical spectrum. Nevertheless, some emission is unaccounted for, possibly due to inaccuracies in the cobalt atomic data. For some supernovae, blueshifts of 1000-3000 km s -1 are seen in infrared and optical features at 3 months. We suggest that this is due to clumping in the ejecta. The evolution of the cobalt/iron mass ratio indicates that 56Co-decay dominates the abundances of these elements. The absolute masses of iron-group elements which we derive support the basic thermonuclear explosion scenario for Type la supernovae. A core-collapse origin is less consistent with our data. © 1997 RAS.
• {Bowers}, E., {Meikle}, W., {Geballe}, T., {Walton}, N., {Pinto}, P., {Dhillon}, V., {Howell}, S., , M. (1997). Infrared and optical spectroscopy of Type IA supernovae in the nebular phase. Monthly Notices Royal Astronomical Society, 290, 663-679.
• {Pinto}, P., , R. (1996). The Physics of Type Ia Supernova Lightcurves: I. Opacity and Diffusion. ArXiv Astrophysics e-prints.
• Eastman, R. G., Woosley, S. E., Weaver, T. A., & Pinto, P. A. (1994). Theoretical light curve of a type IIp supernova. Astrophysical Journal Letters, 430(1), 300-310.
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  Abstract: The light curve and other observable diagnostics are presented for what should be a typical Type II "plateau" supernova, the explosion of a 15 M⊙ red supergiant. The calculations are carried out using a multifrequency radiation transport code that includes opacity from all important mechanisms - bound-bound, bound-free, free-free, and electron scattering. It is found that the inclusion of opacity sources besides electron scattering increases the computed length of the plateau in the 15 M⊙ model by ∼30 days. Especially important is the ultraviolet cutoff caused by a thick forest of lines. Deposition and escape of γ-rays from radioactive decay are also accurately simulated. We find that the presence of 0.06 M⊙ of ejected 56Ni extends the length of the plateau from ∼100 days to ∼140 days. Because of the large hydrogen envelope and radius in this model, mixing does not appreciably alter the bolometric light curve, although it does change the γ-ray light curve significantly. With 0.06 M⊙ of ejected 56Ni, the unmixed (mixed) model peaks in escaping γ-rays at 576 (466) days with a γ-ray luminosity of 3 × 1038 (7 × 1038) ergs s-1. Except for the local group, the γ-rays from an extragalactic 15 M⊙ SNe IIp will be too faint to detect with any existing detectors. However, a Galactic SNe IIp would be quite bright and easily detectable.
• Woosley, S. E., Eastman, R. G., Weaver, T. A., & Pinto, P. A. (1994). SN 1993J: A type IIb supernova. Astrophysical Journal Letters, 429(1), 300-318.
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  Abstract: The evolution of the bright Type II supernova discovered last year in M81, SN 1993J, is consistent with that expected for the explosion of a star which on the main sequence had a mass of 13-16 M⊙ but which, owing to mass exchange with a binary companion (a initially ∼3-5 AU, depending upon the actual presupernova radius and the masses of the two stars) lost almost all of its hydrogen-rich envelope during late helium burning. At the time of explosion, the helium core mass was 4.0 ± 0.5 M⊙ and the hydrogen envelope, 0.20 ± 0.05 M⊙. The envelope was helium and nitrogen-rich (carbon-deficient) and the radius of the star, 4 ± 1 × 1013 cm. The luminosity of the presupernova star was 3 ± 1 × 1038 ergs s-1, with the companion star contributing an additional ∼ 1038 ergs s-1. The star may have been a pulsating variable at the time of the explosion. For an explosion energy near 1051 ergs (KE at infinity) and an assumed distance of 3.3 Mpc, a mass of 56Ni in the range 0.07 ± 0.01 M⊙ was produced and ejected. This prescription gives a light curve which compares favorably with the bolometric observations. Color photometry is more restrictive and requires a model in which the hydrogen-envelope mass is low and the mixing of hydrogen inward has been small, but in which appreciable 56Ni has been mixed outward into the helium and heavy-element core. It is possible to obtain good agreement with B and V light curves during the first 50 days, but later photometry, especially in bands other than B and V, will require a non-LTE spectral calculation for comparison. Based upon our model, we predict a flux of ∼10-5 (3.3 Mpc/D)2 photons cm-2 s-1 in the 847 kcV line of 56Co at peak during 1993 August. It may be easier to detect the Comptonized continuum which peaks at a few times 10-4 photons s-1 cm-2 MeV-1 at 40 keV a few months after the explosion (though neither of these signals were, or should have been, detected by the Compton Gamma-Ray Observatory). The presupernova star was filling its Roche lobe at the time of the explosion and thus its envelope was highly deformed (about 3:2). The companion star is presently embedded in the supernova, but should become visible at age 3 yr (perhaps earlier in the ultraviolet) when the supernova has faded below 1038 ergs s-1. Indeed, if "kicks" have not played an important role, it is still bound to the neutron star.
• {Kuchner}, M., {Kirshner}, R., {Pinto}, P., , B. (1994). Evidence for Ni-56 yields Co-56 yields Fe-56 decay in type IA supernovae. Astrophysical Journal Letters, 426, 89-92.
• {Spyromilio}, J., {Pinto}, P., , R. (1994). On the Origin of the 1.2-MICRON Feature in Type-Ia Supernova Spectra. Monthly Notices of the Royal Astronomical Society, 266, L17.
• {Woosley}, S., {Eastman}, R., {Weaver}, T., , P. (1994). SN 1993J: A Type IIb supernova. Astrophysical Journal, 429, 300-318.
• Eastman, R. G., & Pinto, P. A. (1993). Spectrum formation in supernovae: Numerical techniques. Astrophysical Journal Letters, 412(2), 731-751.
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  Abstract: We have combined several novel techniques for spectrum simulation in the computer program EDDINGTON which solves the comoving frame equation of transfer coupled with the statistical and radiative equilibrium equations. The first of these is a generalization of the accelerated lambda iteration (ALI) scheme to include an approximate frequency-derivative operator. This greatly enhances the convergence rate of ALI in optically thick, high-velocity shear flows. The next is a partial linearization technique which is capable of efficiently solving a very large (∼104) number of rate equations on a moderately sized computer; part of its efficiency derives from a "fixed-excitation" iteration which allows this technique to handle simulations with a large number of (intrinsically) overlapping lines and continua. Finally, we derive an expansion opacity and emissivity approximation which allows us to determine the effect on the transfer and statistical equilibrium of a very large number of lines not explicitly represented in the frequency grid and additionally to treat line-blanketing from species not explicitly included in the rate equations. We illustrate the utility of these techniques with models of two supernovae. The first is a typical Type II supernova 45 days past explosion which illustrates the power of the ALI scheme for optically thick problems in rapidly moving flows. The second is a Type Ia supernova 250 days past explosion which demonstrates the ability of partial linearization and the expansion opacity/emissivity approximation to treat a problem with 727 atomic energy levels coupled by all continua and 4447 lines. For each we discuss rates of convergence and the effect of various convergence-accelerating techniques. Detailed models of various supernovae and the microphysics (e.g., energy deposition and atomic data) we employ will be discussed in future publications.
• Wooden, D. H., Rank, D. M., Bregman, J. D., Witteborn, F. C., Tielens, A. G., Cohen, M., Pinto, P. A., & Axelrod, T. S. (1993). airborne spectrophotometry of SN 1987A from 1.7 to 12.6 microns: time history of the dust continuum and line emission. Astrophysical Journal, Supplement Series, 88(2), 477-507.
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  Abstract: Spectrophotometric observations (1.7-12.6 μm) of SN 1987A from the Kuiper Airborne Observatory are presented for five epochs at 60, 260, 415, 615, and 775 days after the explosion. A variety of emission lines is seen, including members of the hydrogen Humphreys, Pfund, Brackett, and Paschen series, fine-structure lines of metals (including [Ni II] 6.634 μm, [Ni I] 7.507 μm, [Ar II] 6.985 Mm, and [Co II] 10.521 μm), and CO and SiO molecular bands. The temporal evolution of the seven strongest H lines follows case C recombination theory and yields large values of τ(Hα) at 260 and 415 days. A mass of ∼2 × 10-3 M⊙ is derived for stable nickel, and the ratio of the [Ni I] 7.507 μm and [Ni II] 6.634 μm line intensities yields a high ionization fraction of 0.9 in the nickel zone. Dust condensation is clearly detected at 615 days for the first time in a Type II supernova. At no time is there a 9.7 μm emission feature characteristic of interstellar astronomical silicates in the spectra of SN 1987A, nor are the 6.2 or 7.7 μm emission features attributed to polycyclic aromatic hydrocarbons seen. These airborne data are combined with other airborne and ground-based measurements taken at (or near) the same time to form five composite spectra of SN 1987A with wavelength coverage from ∼3200 Å to 100 μm. The IR continuum emission between ∼2 and 100 μm is compared with a three-component model - (1) hot photo-spheric continuum, (2) free-free and free-bound H emission, and (3) dust continuum - with the best fit determined using a nonlinear χ2 method. The dust continuum component is well characterized by a single-temperature graybody emission spectrum, i.e., by the radiation from gray grains or dust in optically thick clumps. At early times (less than 400 days after core collapse), the dust emission tracks the bolometric luminosity at about the 2% level. By 615 days, the fraction of the total luminosity contributed by the IR dust continuum increases dramatically to 0.45, and then to 0.83 at 775 days. We suggest that this dichotomy in the temporal evolution of the dust emission arises from dust with different origins. Circumstellar dust present before the supernova and then heated by it may account for the early emission. Newly condensed dust in the ejecta accounts for the later emission. A lower limit to the dust mass at 775 days is ∼ 10-4 M⊙, but much more dust could be present. Since the emission is well fitted by a graybody, no information on the dust composition can be directly discerned from our data.
• {Eastman}, R., , P. (1993). Spectrum formation in supernovae - Numerical techniques. Astrophysical Journal, 412, 731-751.
• {Wooden}, D., {Rank}, D., {Bregman}, J., {Witteborn}, F., {Tielens}, A., {Cohen}, M., {Pinto}, P., , T. (1993). Airborne spectrophotometry of SN 1987A from 1.7 to 12.6 microns - Time history of the dust continuum and line emission. Astrophysical Journal Supplement, 88, 477-507.
• Leibundgut, B., & Pinto, P. A. (1992). A distance-independent calibration of the luminosity of type Ia supernovae and the hubble constant. Astrophysical Journal Letters, 401(1), 49-59.
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  Abstract: We present a calibration of the absolute magnitude of Type Ia supernovae (SNe Ia) at maximum by means of radioactive decay models for the light curve. Comparison of the calculated late time thermalized radiation with a bolometric light curve constructed from observations circumvents problems of modeling the complex physics that govern the peak phase and avoids the conversion of theoretical luminosities into filter magnitudes. The parameter space for the absolute magnitude is explored with several explosion models and a range of rise times. The absolute B magnitudes at maximum are then used to derive a range for the Hubble constant and the distance to the Virgo Cluster of galaxies from SNe Ia. Critical examination of the Hubble diagram of SNe Ia at peak yields rigorous limits for H0 of 45 and 105 km s-1 Mpc-1. Surprisingly, our determination of the value of H0 is limited strongly by the unknown extinction toward individual supernovae. Improvements on the values of the Hubble constant from SNe Ia remain mainly in spectral modeling to find appropriate explosion models and in the use of near-infrared filters which are affected less by extinction.
• {Leibundgut}, B., , P. (1992). A distance-independent calibration of the luminosity of type IA supernovae and the Hubble constant. Astrophysical Journal, 401, 49-59.
• Leibundgut, B., Kirshner, R. P., Pinto, P. A., Rupen, M. P., Smith, R. C., Gunn, J. E., & Schneider, D. P. (1991). Spectra of two very old supernovae: SN 1986J and SN 1980K. Astrophysical Journal Letters, 372(2), 531-544.
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  Abstract: We present spectra of two aging supernovae, SN 1986J in NGC 891 and SN 1980K in NGC 6946. SN 1986J was observed in 1986 and 1989, ∼4 and ∼7 yr after the explosion, as inferred from radio observations; SN 1980K was observed 1989, 9 years after maximum light. SN 1986J shows two components of emission: narrow lines (Δv < 600 km s-1) of H, He, N, and Fe, and broad lines (Δv > 1000 km s-1) of [O I], [O II, and [O III]. The flux in the narrow Hα has declined by a factor of 10 from 1984 to 1989, while the flux in the broad oxygen lines has not decreased from 1986 to 1989. We attribute these two components to two different emission sites - a circumstellar shell for the narrow lines (already suggested by the very powerful radio emission from SN 1986J) and the actual stellar interior (without hydrogen) for the broad lines. We have developed diagnostics for the oxygen line ratios to estimate the density in the debris as 6 ×108 < nOI, < 2 × 109 at a temperature of 3000 < T < 4000 K. We find that the oxygen debris is highly clumped, filling only 0.001-0.003 of the volume and that the mass of warm neutral oxygen is 0.1 < MOI, < 0.3 M⊙. Overall, the properties of SN 1986J are consistent with the explosion of a massive star with an extensive mass loss. SN 1980K, which was observed at maximum to be a SN II, continues to emit in very broad lines (Δv > 2500 km s-1) of [O I], [O III], [Fe II], and Hα. Comparison with earlier observations suggests that SN 1980K halted its exponential decline in flux in the early 1980s and is now emitting at a constant rate of about 6 × 1037 ergs s-1 in the observed lines. For both SN 1986J and SN 1980K, the underlying energy source sustaining the emission remains uncertain, but continued measurements of the ionization, temperature, and flux may help to distinguish among shocks, radioactivity, pulsar power, or accretion onto a neutron star.
• {Leibundgut}, B., {Kirshner}, R., {Pinto}, P., {Rupen}, M., {Smith}, R., {Gunn}, J., , D. (1991). Spectra of two very old supernovae - SN 1986J and SN 1980K. Astrophysical Journal, 372, 531-544.
• Pinto, P. A. (1989). Detection of space reactors by their gamma-ray and positron emissions. Science & Global Security, 1, 129-146.
• {Witteborn}, F., {Bregman}, J., {Wooden}, D., {Pinto}, P., {Rank}, D., {Woosley}, S., , M. (1989). Spectral line profiles of nickel and argon in supernova 1987A - Expansion velocity and electron scattering effects. Astrophysical Journal Letters, 338, L9-L12.
• {Woosley}, S., {Hartmann}, D., , P. (1989). Hard emission at late times from SN 1987A. Astrophysical Journal, 346, 395-404.
• Pinto, P. A., & Woosley, S. E. (1988). The theory of gamma-ray emergence in supernova 1987A. Nature, 333(6173), 534-537.
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  Abstract: Since June 1987 we have had little cause to doubt the presence of radioactivity in supernova 1987A. The optical light curve has tracked the 77.1-day half-life of 56Co to better than 1% (refs 1-3), at least through November, demonstrating conclusively the synthesis of 0.075Ṁ of radioactive 56Ni in the explosion4. It was anticipated that the decay of 56Co to 56Fe would give rise to detectable γ-ray line emission5,6 at 847 and 1,238 keV with a peak flux7 of 10-3 photons cm-2 s-1 about one year after the explosion. Many calculations of the light curves for these lines were made for the particular case of SN1987A (refs 8-14), and in August, both lines were detected15-18, with a strength within a factor of two of 10-3 photons cm-2 s-1, but about six months earlier than predicted (see ref. 8 for example). Here we show that the early emergence of γ-rays can be accounted for in a 'mixed' model, in which an approximately isotropic process destroys chemical segregation with respect to radial mass coordinate and velocity. © 1988 Nature Publishing Group.
• Rank, D. M., Pinto, P. A., Woosley, S. E., Bregman, J. D., Wittebornt, F. C., Axelrod, T. S., & Cohen, M. (1988). Nickel, argon and cobalt in the infrared spectrum of SN1987A: The core becomes visible. Nature, 331(6156), 505-506.
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  Abstract: Infrared spectra of supernova 1987A taken in April and November 1987 from the Kuiper Airborne Observatory (KAO) show two distinctly different stages in the evolution of the expanding gas shell. In April both the optical and infrared spectrum originated from the hydrogen envelope, the still opaque remnant of the outer regions of the progenitor star's atmosphere. This region of the star was presumably of near solar chemical composition (although the elements heavier than helium are expected to have had an abundance from two to four times less than the Sun). Our April spectrum shows weak hydrogen lines rising above a 5,000-K photospheric continuum, in good agreement with this picture. By November, however, the spectrum of SN1987A had changed dramatically. Strong emission lines from heavy elements as well as many lines from highly excited levels of hydrogen dominated the spectrum with peak flux levels in the lines at or slightly above the level of the continuum in April. The intensity of these lines and the abundances of the heavy elements inferred from them demonstrate that the inner regions of the supernova are just now becoming visible at infrared wavelengths. These regfons are expected to contain heavy elements produced by advanced nuclear burning stages in the progenitor star (Sk-69 202) and in the shock wave that ejected all material external to the iron core. They are, of course, very deficient in hydrogen. © 1988 Nature Publishing Group.
• {Pinto}, P., , S. (1988). The theory of gamma-ray emergence in supernova 1987A. Nature, 333, 534-537.
• {Pinto}, P., , S. (1988). X-ray and gamma-ray emission from supernova 1987A. Astrophysical Journal, 329, 820-830.
• {Pinto}, P., {Woosley}, S., , L. (1988). SN 1987A - Out on the tail. Astrophysical Journal Letters, 331, L101-L104.
• {Rank}, D., {Pinto}, P., {Woosley}, S., {Bregman}, J., , F. (1988). Nickel, argon and cobalt in the infrared spectrum of SN1987A - The core becomes visible. Nature, 331, 505.
• {Witteborn}, F., {Bregman}, J., {Wooden}, D., {Pinto}, P., {Rank}, D., , M. (1988). Supernova 1987A in the Large Magellanic Cloud. IAU Circular, 4592.
• {Woosley}, S., {Pinto}, P., , L. (1988). Supernova 1987A - Six weeks later. Astrophysical Journal, 324, 466-489.
• {Woosley}, S., {Pinto}, P., , T. (1988). Recent results on SN 1987A. Proceedings of the Astronomical Society of Australia, 7, 355-370.
• {Woosley}, S., {Pinto}, P., {Martin}, P., , T. (1987). Supernova 1987A in the Large Magellanic Cloud - The explosion of an approximately 20 solar mass star which has experienced mass loss?. Astrophysical Journal, 318, 664-673.
• {De Robertis}, M., , P. (1985). Spectrophotometry of the supernova 1983u in NGC 3227. Astrophysical Journal Letters, 293, L77-L81.
• {Mallama}, A., {Skillman}, D., {Pinto}, P., , B. (1977). Minima of Eclipsing Variables. Information Bulletin on Variable Stars, 1249.
• {Ney}, E., {Stoddart}, J., {Hubbard}, R., , P. (1976). Nova Vulpeculae 1976. IAU Circular, 3023.

Proceedings Publications

• Ferrer, D., Eisenstein, D., Metchnik, M. V., & Pinto, P. A. (2014, jan). Faster, Better, Cheaper N-Body with Abacus. In American Astronomical Society Meeting Abstracts, 223, #457.15.
• {Ferrer}, D., {Eisenstein}, D., {Metchnik}, M., , P. (2014, jan). Faster, Better, Cheaper N-Body with Abacus. In American Astronomical Society Meeting Abstracts \#223, 223.
• {Eisenstein}, D., {Blanton}, M., {Cuesta}, A., {Eckel}, J., {Mehta}, K., {Metchnik}, M., {Padmanabhan}, N., {Percival}, W., {Pinto}, P., {Reid}, B., {Schlegel}, D., {Seo}, H., {Sirko}, E., {Spergel}, D., {White}, M., , X. (2012, feb). Dark Energy and Cosmic Sound. In IAC Talks, Astronomy and Astrophysics Seminars from the Instituto de Astrof{\'{\i}}sica de Canarias.
• {Mehta}, K., {Seo}, H., {Eckel}, J., {Eisenstein}, D., {Metchnik}, M., {Pinto}, P., , X. (2011, may). Galaxy Bias and its Effects on the Baryon Acoustic Oscillations Measurements. In American Astronomical Society Meeting Abstracts \#218, 43.
• {Xu}, X., {Eckel}, J., {Eisenstein}, D., {Metchnik}, M., {Padmanabhan}, N., {Pinto}, P., {Seo}, H., , M. (2011, may). Baryon Acoustic Oscillations Analysis Techniques. In American Astronomical Society Meeting Abstracts \#218, 43.
• Ivezic}, Z., {Axelrod}, T., {Burke}, D., {Claver}, C., {Connolly}, A., {Cook}, K., {Gilmore}, K., {Jones}, L., {Kahn}, S., {Lopez}, S., {Lupton}, R., {Monet}, D., {Pinto}, P., {Saha}, A., {Scranton}, R., {Smith}, C., {Strauss}, M., {Stubbs}, C., {Sweeney}, D., , {Szalay}, A., et al. (2010, jan). LSST: from Science Drivers to Data Products. In American Astronomical Society Meeting Abstracts \#215, 42.
• {Krabbendam}, V., {Chandrasekharan}, S., {Cook}, K., {Ivezic}, Z., {Jones}, R., {Krughoff}, K., {Miller}, M., {Petry}, C., {Pinto}, P., {Ridgway}, S., , A. (2010, jan). LSST Operations Simulator. In American Astronomical Society Meeting Abstracts \#215, 42.
• Cook}, K., {Pinto}, P., {Delgado}, F., {Miller}, M., {Petry}, C., {Saha}, A., {Gee}, P., {Tyson}, J., {Ivezic}, Z., {Jones}, L., & Collaboration, {. (2009, jan). LSST: Cadence Design and Simulation. In American Astronomical Society Meeting Abstracts \#213, 41.
• Ivezic}, Z., {Tyson}, J., {Axelrod}, T., {Burke}, D., {Claver}, C., {Cook}, K., {Kahn}, S., {Lupton}, R., {Monet}, D., {Pinto}, P., {Strauss}, M., {Stubbs}, C., {Jones}, L., {Saha}, A., {Scranton}, R., {Smith}, C., & Collaboration, {. (2009, jan). LSST: From Science Drivers To Reference Design And Anticipated Data Products. In American Astronomical Society Meeting Abstracts \#213, 41.
• Wood-Vasey}, W., {Olivier}, S., {Cinabro}, D., {Zhan}, H., {Biswas}, R., {Wang}, Y., {Pinto}, P., {Wang}, L., & Collaboration, {. S. (2009, jan). Cosmology, Clusters, and Chemistry: How Supernovae Trace and Shape The Universe. In American Astronomical Society Meeting Abstracts \#213, 41.
• {Ivezi{\'c}}, {. Z., {Axelrod}, T., {Becker}, A., {Becla}, J., {Borne}, K., {Burke}, D., {Claver}, C., {Cook}, K., {Connolly}, A., {Gilmore}, D., {Jones}, R., {Juri{\'c}}, M., {Kahn}, S., {Lim}, K., {Lupton}, R., {Monet}, D., {Pinto}, P., {Sesar}, B., {Stubbs}, C., , J. (2008, dec). Parametrization and Classification of 20 Billion LSST Objects: Lessons from SDSS. In American Institute of Physics Conference Series, 1082.
• {Ivezi{\'c}}, {. Z., {Monet}, D., {Bond}, N., {Juri{\'c}}, M., {Sesar}, B., {Munn}, J., {Lupton}, R., {Gunn}, J., {Knapp}, G., {Tyson}, A., {Pinto}, P., , K. (2008, jul). Astrometry with digital sky surveys: from SDSS to LSST. In A Giant Step: from Milli- to Micro-arcsecond Astrometry, 248.
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Others

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• {Pinto}, P. (1988). The late-time spectra of supernovae.