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Massimo Marengo

Bio: Massimo Marengo is an academic researcher from Iowa State University. The author has contributed to research in topics: Spitzer Space Telescope & Stars. The author has an hindex of 52, co-authored 228 publications receiving 13242 citations. Previous affiliations of Massimo Marengo include University of Arizona & International School for Advanced Studies.


Papers
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Journal ArticleDOI
TL;DR: The Infrared Array Camera (IRAC) is one of three focal plane instruments on the Spitzer Space Telescope as mentioned in this paper, which is a four-channel camera that obtains simultaneous broadband images at 3.6, 4.5, 5.8, and 8.0 m.
Abstract: The Infrared Array Camera (IRAC) is one of three focal plane instruments on the Spitzer Space Telescope. IRAC is a four-channel camera that obtains simultaneous broadband images at 3.6, 4.5, 5.8, and 8.0 � m. Two nearly adjacent 5A2 ; 5A2 fields of view in the focal plane are viewed by the four channels in pairs (3.6 and 5.8 � m; 4.5 and 8 � m). All four detector arrays in the camera are 256 ; 256 pixels in size, with the two shorter wavelength channels using InSb and the two longer wavelength channels using Si:As IBC detectors. IRAC is a powerful survey instrument because of its high sensitivity, large field of view, and four-color imaging. This paper summarizes the in-flight scientific, technical, and operational performance of IRAC.

3,567 citations

Journal ArticleDOI
Sergio Molinari1, B. Swinyard, John Bally2, M. J. Barlow3, J.-P. Bernard4, Paul Martin5, Toby J. T. Moore6, Alberto Noriega-Crespo7, Rene Plume8, Leonardo Testi9, Leonardo Testi1, Annie Zavagno10, Alain Abergel11, Babar Ali7, L. D. Anderson10, Ph. André12, J.-P. Baluteau10, Cara Battersby2, M. T. Beltrán1, M. Benedettini1, N. Billot7, J. A. D. L. Blommaert13, Sylvain Bontemps12, Sylvain Bontemps14, F. Boulanger11, Jan Brand1, Christopher M. Brunt15, Michael G. Burton16, Luca Calzoletti, Sean Carey7, Paola Caselli17, Riccardo Cesaroni1, José Cernicharo18, Sukanya Chakrabarti, Antonio Chrysostomou, Martin Cohen, Mathieu Compiegne5, P. de Bernardis19, G. de Gasperis20, A. M. di Giorgio1, Davide Elia1, F. Faustini, Nicolas Flagey7, Yasuo Fukui21, Gary A. Fuller22, K. Ganga23, Pedro García-Lario, Jason Glenn2, Paul F. Goldsmith24, Matthew Joseph Griffin25, Melvin Hoare17, Maohai Huang26, D. Ikhenaode19, C. Joblin4, G. Joncas27, Mika Juvela28, Jason M. Kirk25, Guilaine Lagache11, Jin-Zeng Li26, T. L. Lim, S. D. Lord7, Massimo Marengo29, Douglas J. Marshall4, Silvia Masi19, Fabrizio Massi1, Mikako Matsuura3, Vincent Minier12, Marc-Antoine Miville-Deschenes11, L. Montier4, L. K. Morgan6, Frédérique Motte12, Joseph C. Mottram15, T. G. Müller30, Paolo Natoli20, J. Neves31, Luca Olmi1, Roberta Paladini7, Deborah Paradis7, Harriet Parsons31, Nicolas Peretto22, Nicolas Peretto12, M. R. Pestalozzi1, Stefano Pezzuto1, F. Piacentini19, Lorenzo Piazzo19, D. Polychroni1, M. Pomarès10, Cristina Popescu30, William T. Reach7, Isabelle Ristorcelli4, Jean-François Robitaille27, Thomas P. Robitaille29, J. A. Rodón10, A. Roy5, Pierre Royer13, D. Russeil10, Paolo Saraceno1, Marc Sauvage12, Peter Schilke32, Eugenio Schisano1, Nicola Schneider12, Frederic Schuller, Benjamin L. Schulz7, B. Sibthorpe25, Hazel Smith29, Michael D. Smith33, L. Spinoglio1, Dimitrios Stamatellos25, Francesco Strafella, Guy S. Stringfellow2, E. Sturm30, R. Taylor8, Mark Thompson31, Alessio Traficante20, Richard J. Tuffs30, Grazia Umana1, Luca Valenziano1, R. Vavrek, M. Veneziani19, Serena Viti3, C. Waelkens13, Derek Ward-Thompson25, Glenn J. White34, L. A. Wilcock25, Friedrich Wyrowski, Harold W. Yorke24, Qizhou Zhang29 
TL;DR: In this paper, the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key program that will map the inner Galactic plane of the Milky Way in 5 bands, were presented.
Abstract: We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key program that will map the inner Galactic plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2° × 2° tiles approximately centered at l = 30° and l = 59°. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around AV ~ 1 is exceeded for the regions in the l = 59° field; a AV value between 5 and 10 is found for the l = 30° field, likely due to the relatively higher distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.

752 citations

Journal ArticleDOI
Sergio Molinari, B. Swinyard, John Bally, M. J. Barlow, J.-P. Bernard, Paul Martin, Toby J. T. Moore, Alberto Noriega-Crespo, Rene Plume, Leonardo Testi, Annie Zavagno, A. Abergel, Babar Ali, L. D. Anderson, Pascal André, Jean-Paul Baluteau, Cara Battersby, M. T. Beltrán, M. Benedettini, N. Billot, J. A. D. L. Blommaert, Sylvain Bontemps, F. Boulanger, Jan Brand, Christopher M. Brunt, Michael G. Burton, Luca Calzoletti, Sean Carey, Paola Caselli, Riccardo Cesaroni, José Cernicharo, Sukanya Chakrabarti, Antonio Chrysostomou, Martin Cohen, Mathieu Compiegne, P. de Bernardis, G. de Gasperis, A. M. di Giorgio, Davide Elia, F. Faustini, Nicolas Flagey, Yasuo Fukui, Gary A. Fuller, K. Ganga, Pedro García-Lario, Jason Glenn, Paul F. Goldsmith, Matthew Joseph Griffin, Melvin Hoare, Maohai Huang, D. Ikhenaode, C. Joblin, G. Joncas, Mika Juvela, Jason M. Kirk, Guilaine Lagache, Jin-Zeng Li, T. L. Lim, S. D. Lord, Massimo Marengo, D. J. Marshall, Silvia Masi, Fabrizio Massi, Mikako Matsuura, Vincent Minier, Marc-Antoine Miville-Deschenes, L. Montier, L. K. Morgan, Frédérique Motte, Joseph C. Mottram, T. Mueller, Paolo Natoli, J. Neves, Luca Olmi, R. Paladini, D. Paradis, Harriet Parsons, Nicolas Peretto, M. R. Pestalozzi, Stefano Pezzuto, F. Piacentini, Lorenzo Piazzo, D. Polychroni, M. Pomarès, Cristina Popescu, William T. Reach, Isabelle Ristorcelli, Jean-François Robitaille, Thomas P. Robitaille, J. A. Rodón, A. Roy, Pierre Royer, D. Russeil, P. Saraceno, Marc Sauvage, Peter Schilke, Eugenio Schisano, Nicola Schneider, Frederic Schuller, Benjamin L. Schulz, B. Sibthorpe, Howard A. Smith, Michael D. Smith, L. Spinoglio, Dimitrios Stamatellos, Francesco Strafella, Guy S. Stringfellow, E. Sturm, Russell H. Taylor, Maggie A. Thompson, Alessio Traficante, Richard J. Tuffs, Grazia Umana, Luca Valenziano, R. Vavrek, M. Veneziani, Serena Viti, C. Waelkens, Derek Ward-Thompson, Glenn J. White, L. A. Wilcock, Friedrich Wyrowski, H. W. Yorke, Qizhou Zhang 
TL;DR: In this paper, the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key-project that will map the inner Galactic Plane of the Milky Way in 5 bands are presented.
Abstract: We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key-project that will map the inner Galactic Plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2{\deg} x 2{\deg} tiles approximately centered at l=30{\deg} and l=59{\deg}. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call 'cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around A_V of about 1 is exceeded for the regions in the l=59{\deg} field; a A_V value between 5 and 10 is found for the l=30{\deg} field, likely due to the relatively larger distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.

735 citations

Journal ArticleDOI
TL;DR: The Infrared Array Camera (IRAC) on the Spitzer Space Telescope is absolutely calibrated by comparing photometry of a set of A stars near the north ecliptic pole to predictions based on ground-based observations and a stellar atmosphere model as mentioned in this paper.
Abstract: The Infrared Array Camera (IRAC) on the Spitzer Space Telescope is absolutely calibrated by comparing photometry of a set of A stars near the north ecliptic pole to predictions based on ground‐based observations and a stellar atmosphere model The brightness of point sources is calibrated to an accuracy of 3%, relative to models for A‐star stellar atmospheres, for observations performed and analyzed in the same manner as for the calibration stars This includes corrections for the location of the star in the array and the location of the centroid within the peak pixel Long‐term stability of the IRAC photometry was measured by monitoring the brightness of A dwarfs and K giants (near the north ecliptic pole) observed several times per month; the photometry is stable to 15% (rms) over a year Intermediate‐timescale stability of the IRAC photometry was measured by monitoring at least one secondary calibrator (near the ecliptic plane) every 12 hr while IRAC was in nominal operations; the intermediat

681 citations

Journal ArticleDOI
Sergio Molinari, B. Swinyard, John Bally, M. J. Barlow, J.-P. Bernard, Pierrick Martin, Toby J. T. Moore, Alberto Noriega-Crespo, Rene Plume, Leonardo Testi, Annie Zavagno, A. Abergel, Babar Ali, Pascal André, Jean-Paul Baluteau, M. Benedettini, Olivier Berné, N. Billot, J. A. D. L. Blommaert, Sylvain Bontemps, F. Boulanger, Jan Brand, Christopher M. Brunt, Michael G. Burton, L. Campeggio, Sean Carey, Paola Caselli, Riccardo Cesaroni, José Cernicharo, Sukanya Chakrabarti, Antonio Chrysostomou, C. Codella, Martin Cohen, Mathieu Compiegne, C. J. Davis, P. de Bernardis, G. de Gasperis, J. Di Francesco, A. M. di Giorgio, Davide Elia, F. Faustini, J. Fischera, Yasuo Fukui, Gary A. Fuller, K. Ganga, Pedro García-Lario, M. Giard, Giovanna Giardino, Jason Glenn, Paul F. Goldsmith, Matthew Joseph Griffin, Melvin Hoare, Maohai Huang, Biwei Jiang, C. Joblin, G. Joncas, Mika Juvela, Jason M. Kirk1, Guilaine Lagache, Jin-Zeng Li, T. L. Lim, S. D. Lord, Philip W. Lucas, B. Maiolo, Massimo Marengo, D. J. Marshall, Silvia Masi, Fabrizio Massi, Mikako Matsuura, C. Meny, Vincent Minier, Marc-Antoine Miville-Deschenes, L. Montier, Frédérique Motte, Thomas G. Müller1, Paolo Natoli, J. Neves, Luca Olmi, R. Paladini, D. Paradis, M. R. Pestalozzi, Stefano Pezzuto, F. Piacentini, M. Pomarès, Cristina Popescu1, William T. Reach, John Richer, Isabelle Ristorcelli, A. Roy, Pierre Royer, D. Russeil, Paolo Saraceno, Marc Sauvage, Peter Schilke, N. Schneider-Bontemps, Frederic Schuller, B. Schultz, D. S. Shepherd, B. Sibthorpe, Howard A. Smith, Michael D. Smith, L. Spinoglio, Dimitrios Stamatellos, Francesco Strafella, Guy S. Stringfellow, E. Sturm1, Russell H. Taylor, Maggie A. Thompson, Richard J. Tuffs1, Grazia Umana, Luca Valenziano, R. Vavrek, Serena Viti, C. Waelkens, Derek Ward-Thompson, Glenn J. White, Friedrich Wyrowski, H. W. Yorke, Qizhou Zhang 
TL;DR: Hi-GAL as mentioned in this paper is an open-time key project of the Herschel Space Observatory, which aims to detect the earliest phases of the formation of molecular clouds and high-mass stars.
Abstract: Hi-GAL, the Herschel infrared Galactic Plane Survey, is an Open Time Key Project of the Herschel Space Observatory. It will make an unbiased photometric survey of the inner Galactic plane by mapping a 2° wide strip in the longitude range ∣l∣ < 60° in five wavebands between 70 μm and 500 μm. The aim of Hi-GAL is to detect the earliest phases of the formation of molecular clouds and high-mass stars and to use the optimum combination of Herschel wavelength coverage, sensitivity, mapping strategy, and speed to deliver a homogeneous census of star-forming regions and cold structures in the interstellar medium. The resulting representative samples will yield the variation of source temperature, luminosity, mass and age in a wide range of Galactic environments at all scales from massive YSOs in protoclusters to entire spiral arms, providing an evolutionary sequence for the formation of intermediate and high-mass stars. This information is essential to the formulation of a predictive global model of the role of environment and feedback in regulating the star-formation process. Such a model is vital to understanding star formation on galactic scales and in the early universe. Hi-GAL will also provide a science legacy for decades to come with incalculable potential for systematic and serendipitous science in a wide range of astronomical fields, enabling the optimum use of future major facilities such as JWST and ALMA.

579 citations


Cited by
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Journal ArticleDOI
TL;DR: In this article, the Wilkinson Microwave Anisotropy Probe (WMAP) 5-year data were used to constrain the physics of cosmic inflation via Gaussianity, adiabaticity, the power spectrum of primordial fluctuations, gravitational waves, and spatial curvature.
Abstract: The Wilkinson Microwave Anisotropy Probe (WMAP) 5-year data provide stringent limits on deviations from the minimal, six-parameter Λ cold dark matter model. We report these limits and use them to constrain the physics of cosmic inflation via Gaussianity, adiabaticity, the power spectrum of primordial fluctuations, gravitational waves, and spatial curvature. We also constrain models of dark energy via its equation of state, parity-violating interaction, and neutrino properties, such as mass and the number of species. We detect no convincing deviations from the minimal model. The six parameters and the corresponding 68% uncertainties, derived from the WMAP data combined with the distance measurements from the Type Ia supernovae (SN) and the Baryon Acoustic Oscillations (BAO) in the distribution of galaxies, are: Ω b h 2 = 0.02267+0.00058 –0.00059, Ω c h 2 = 0.1131 ± 0.0034, ΩΛ = 0.726 ± 0.015, ns = 0.960 ± 0.013, τ = 0.084 ± 0.016, and at k = 0.002 Mpc-1. From these, we derive σ8 = 0.812 ± 0.026, H 0 = 70.5 ± 1.3 km s-1 Mpc–1, Ω b = 0.0456 ± 0.0015, Ω c = 0.228 ± 0.013, Ω m h 2 = 0.1358+0.0037 –0.0036, z reion = 10.9 ± 1.4, and t 0 = 13.72 ± 0.12 Gyr. With the WMAP data combined with BAO and SN, we find the limit on the tensor-to-scalar ratio of r 1 is disfavored even when gravitational waves are included, which constrains the models of inflation that can produce significant gravitational waves, such as chaotic or power-law inflation models, or a blue spectrum, such as hybrid inflation models. We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and the spatial curvature of the universe: –0.14 < 1 + w < 0.12(95%CL) and –0.0179 < Ω k < 0.0081(95%CL). We provide a set of WMAP distance priors, to test a variety of dark energy models with spatial curvature. We test a time-dependent w with a present value constrained as –0.33 < 1 + w 0 < 0.21 (95% CL). Temperature and dark matter fluctuations are found to obey the adiabatic relation to within 8.9% and 2.1% for the axion-type and curvaton-type dark matter, respectively. The power spectra of TB and EB correlations constrain a parity-violating interaction, which rotates the polarization angle and converts E to B. The polarization angle could not be rotated more than –59 < Δα < 24 (95% CL) between the decoupling and the present epoch. We find the limit on the total mass of massive neutrinos of ∑m ν < 0.67 eV(95%CL), which is free from the uncertainty in the normalization of the large-scale structure data. The number of relativistic degrees of freedom (dof), expressed in units of the effective number of neutrino species, is constrained as N eff = 4.4 ± 1.5 (68%), consistent with the standard value of 3.04. Finally, quantitative limits on physically-motivated primordial non-Gaussianity parameters are –9 < f local NL < 111 (95% CL) and –151 < f equil NL < 253 (95% CL) for the local and equilateral models, respectively.

5,904 citations

Journal ArticleDOI
TL;DR: In this paper, the authors present cosmological parameter constraints based on the final nine-year WMAP data, in conjunction with a number of additional cosmology data sets.
Abstract: We present cosmological parameter constraints based on the final nine-year WMAP data, in conjunction with a number of additional cosmological data sets. The WMAP data alone, and in combination, continue to be remarkably well fit by a six-parameter CDM model. When WMAP data are combined with measurements of the high-l cosmic microwave background (CMB) anisotropy, the baryon acoustic oscillation (BAO) scale, and the Hubble constant, the matter and energy densities, bh 2 , ch 2 , and , are each determined to a precision of 1.5%. The amplitude of the primordial spectrum is measured to within 3%, and there is now evidence for a tilt in the primordial spectrum at the 5 level, confirming the first detection of tilt based on the five-year WMAP data. At the end of the WMAP mission, the nine-year data decrease the allowable volume of the six-dimensional CDM parameter space by a factor of 68,000 relative to pre-WMAP measurements. We investigate a number of data combinations and show that their CDM parameter fits are consistent. New limits on deviations from the six-parameter model are presented, for example: the fractional contribution of tensor modes is limited to r < 0.13 (95% CL); the spatial curvature parameter is limited to k = 0.0027 +0.0039 0.0038 ; the summed mass of neutrinos is limited to P m < 0.44 eV (95% CL); and the number of relativistic species is found to lie within Ne = 3.84±0.40, when the full data are analyzed. The joint constraint on Ne and the primordial helium abundance, YHe, agrees with the prediction of standard Big Bang nucleosynthesis. We compare recent Planck measurements of the Sunyaev‐Zel’dovich eect with our seven-year measurements, and show their mutual agreement. Our analysis of the polarization pattern around temperature extrema is updated. This confirms a fundamental prediction of the standard cosmological model and provides a striking illustration of acoustic oscillations and adiabatic initial conditions in the early universe. Subject headings: cosmic microwave background, cosmology: observations, early universe, dark matter, space vehicles, space vehicles: instruments, instrumentation: detectors, telescopes

5,488 citations

Journal ArticleDOI
TL;DR: The Spitzer Space Telescope, NASA's great Observatory for infrared astronomy, was launched 2003 August 25 and is returning excellent scientific data from its Earth-trailing solar orbit as mentioned in this paper.
Abstract: The Spitzer Space Telescope, NASA's Great Observatory for infrared astronomy, was launched 2003 August 25 and is returning excellent scientific data from its Earth-trailing solar orbit. Spitzer combines the intrinsic sensitivity achievable with a cryogenic telescope in space with the great imaging and spectroscopic power of modern detector arrays to provide the user community with huge gains in capability for exploration of the cosmos in the infrared. The observatory systems are largely performing as expected, and the projected cryogenic lifetime is in excess of 5 years. This paper summarizes the on-orbit scientific, technical, and operational performance of Spitzer. Subsequent papers in this special issue describe the Spitzer instruments in detail and highlight many of the exciting scientific results obtained during the first 6 months of the Spitzer mission.

3,177 citations

Journal ArticleDOI
TL;DR: In this paper, the authors review progress over the past decade in observations of large-scale star formation, with a focus on the interface between extragalactic and Galactic studies.
Abstract: We review progress over the past decade in observations of large-scale star formation, with a focus on the interface between extragalactic and Galactic studies. Methods of measuring gas contents and star-formation rates are discussed, and updated prescriptions for calculating star-formation rates are provided. We review relations between star formation and gas on scales ranging from entire galaxies to individual molecular clouds.

2,525 citations

Journal ArticleDOI
TL;DR: The Multiband Imaging Photometer for Spitzer (MIPS) as discussed by the authors provides long-wavelength capability for the mission in imaging bands at 24, 70, and 160?m and measurements of spectral energy distributions between 52 and 100?m at a spectral resolution of about 7%.
Abstract: The Multiband Imaging Photometer for Spitzer (MIPS) provides long-wavelength capability for the mission in imaging bands at 24, 70, and 160 ?m and measurements of spectral energy distributions between 52 and 100 ?m at a spectral resolution of about 7%. By using true detector arrays in each band, it provides both critical sampling of the Spitzer point-spread function and relatively large imaging fields of view, allowing for substantial advances in sensitivity, angular resolution, and efficiency of areal coverage compared with previous space far-infrared capabilities. The 24 ?m array has excellent photometric properties, and measurements with rms relative errors of about 1% can be obtained. The two longer-wavelength arrays use detectors with poor photometric stability, but a system of onboard stimulators used for relative calibration, combined with a unique data pipeline, produce good photometry with rms relative errors of less than 10%.

2,370 citations