Grid Data Source Engine: Grid gateway to the Virtual Observatory
… and Systems XV, 2006
... Baruffolo2, Fabio ~ Leopoldo Benacchio2 Istituto Nazioriale di Astrofisica, 00136 Rome, Italy... more ... Baruffolo2, Fabio ~ Leopoldo Benacchio2 Istituto Nazioriale di Astrofisica, 00136 Rome, ItalyEdgardo Ambrosi, Antonia ... Catalog and the the archive of observational data from the Italian Galileo National ... X, ed. FR Harnden, Jr., FA Primini, & HE Payne (San Francisco: ASP), 160 ...
The Euclid mission – with its spectroscopic galaxy survey covering a sky area over 15 000 deg2 in... more The Euclid mission – with its spectroscopic galaxy survey covering a sky area over 15 000 deg2 in the redshift range 0.9 < z < 1.8 – will provide a sample of tens of thousands of cosmic voids. This paper thoroughly explores for the first time the constraining power of the void size function on the properties of dark energy (DE) from a survey mock catalogue, the official Euclid Flagship simulation. We identified voids in the Flagship light-cone, which closely matches the features of the upcoming Euclid spectroscopic data set. We modelled the void size function considering a state-of-the art methodology: we relied on the volume-conserving (Vdn) model, a modification of the popular Sheth & van de Weygaert model for void number counts, extended by means of a linear function of the large-scale galaxy bias. We found an excellent agreement between model predictions and measured mock void number counts. We computed updated forecasts for the Euclid mission on DE from the void size func...
The large infrastructure projects for the next decade will allow a new quantum leap in terms of n... more The large infrastructure projects for the next decade will allow a new quantum leap in terms of new possible science. ESFRI, the European Strategy Forum on Research Infrastructures, a strategic initiative to develop the scientific integration of Europe, has identified four facilities (SKA, CTA, KM3Net and E-ELT) deserving priority in support. The ASTERICS project aims to address the cross-cutting synergies and common challenges shared by the various Astronomy ESFRI and other world-class facilities. The project (22 partners across Europe) is funded by the EU Horizon 2020 programme with 15 MEuro in 4 years. It brings together for the first time the astronomy, astrophysics and particle astrophysics communities, in addition to other related research infrastructures.
The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic ... more The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of i ∼ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage iv dark energy projects, particularly Euclid and the Nancy Grace Roman Space Telescope (Roman), which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B–2019B semesters using the DEIMOS, LRIS, and MOSFIRE multiobject spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 < z p < 2.6 range of interest for the Euclid cosmological goals, then with the current data release, C3R2 has increased t...
We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, upd... more We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, updating the calculation presented in the Euclid Red Book in several ways. We account for revisions to the Euclid near-infrared filter wavelengths; we adopt steeper rates of decline of the quasar luminosity function (QLF; Φ) with redshift, Φ ∝ 10k(z − 6), k = −0.72, and a further steeper rate of decline, k = −0.92; we use better models of the contaminating populations (MLT dwarfs and compact early-type galaxies); and we make use of an improved Bayesian selection method, compared to the colour cuts used for the Red Book calculation, allowing the identification of fainter quasars, down to JAB ∼ 23. Quasars at z > 8 may be selected from Euclid OYJH photometry alone, but selection over the redshift interval 7 < z < 8 is greatly improved by the addition of z-band data from, e.g., Pan-STARRS and LSST. We calculate predicted quasar yields for the assumed values of the rate of decline o...
Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at ... more Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible
Proceedings of the International Astronomical Union, 2014
Euclid is the next ESA mission devoted to cosmology. It aims at observing most of the extragalact... more Euclid is the next ESA mission devoted to cosmology. It aims at observing most of the extragalactic sky, studying both gravitational lensing and clustering over ~15,000 square degrees. The mission is expected to be launched in year 2020 and to last six years. The sheer amount of data of different kinds, the variety of (un)known systematic effects and the complexity of measures require efforts both in sophisticated simulations and techniques of data analysis. We review the mission main characteristics, some aspects of the the survey and highlight some of the areas of interest to this meeting.
Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in... more Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization
Planck intermediate results. XXVI. Optical identification and redshifts of Planck clusters with t... more Planck intermediate results. XXVI. Optical identification and redshifts of Planck clusters with the RTT150 telescope
Publications of the Astronomical Society of the Pacific, 2008
In order to offer an intuitive but effective access to a growing number of cosmological simulatio... more In order to offer an intuitive but effective access to a growing number of cosmological simulations, we have developed the Italian Theoretical Virtual Observatory project (ITVO), as described by Pasian and colleagues in 2006. In this work we describe two Web portals as two ways to access and share complex data coming from numerical astrophysical simulations. We present a set of Web services aimed at offering services such as Simple Numeric Access (ProtocolSNAPSimple Numeric Access Protocol), as described by Gheller and colleagues in 2006, and Randomizers dealing with different data formats. The Web services technology allows us to run a particular task (a SNAP job, for instance) close to its data, avoiding an expensive data transfer.
Monthly Notices of the Royal Astronomical Society, 2010
QUICK DETECTION SYSTEM or QDS is a software package that has been developed for detecting point s... more QUICK DETECTION SYSTEM or QDS is a software package that has been developed for detecting point sources in the Planck satellite data as soon as the data become available, a few days after transmission to the Earth. Point sources are detected by filtering the data with a filter defined by the Mexican hat wavelet. An alert is generated on those detections that are found to be interesting, such as prominent flaring, according to the criteria specified to the software. The goal is to detect spectral or flux variability in active galactic nuclei so that instant multifrequency follow-up observations with other instruments could be arranged to study the interesting behaviour.
We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applyi... more We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 100 to 857 GHz frequency channel maps from the Planck survey. This map shows an obvious galaxy cluster tSZ signal that is well matched with blindly detected clusters in the Planck SZ catalogue. To characterize the signal in the tSZ map we have computed its angular power spectrum. At large angular scales (< 60), the major foreground contaminant is the diffuse thermal dust emission. At small angular scales (> 500) the clustered cosmic infrared background and residual point sources are the major contaminants. These foregrounds are carefully modelled and subtracted. We thus measure the tSZ power spectrum over angular scales 0.17 • < ∼ θ < ∼ 3.0 • that were previously unexplored. The measured tSZ power spectrum is consistent with that expected from the Planck catalogue of SZ sources, with clear evidence of additional signal from unresolved clusters and, potentially, diffuse warm baryons. Marginalized band-powers of the Planck tSZ power spectrum and the best-fit model are given. The non-Gaussianity of the Compton parameter map is further characterized by computing its 1D probability distribution function and its bispectrum. The measured tSZ power spectrum and high order statistics are used to place constraints on σ 8 .
We present constraints on cosmological parameters using number counts as a function of redshift f... more We present constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude σ 8 and matter density parameter Ω m in a flat ΛCDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that σ 8 = 0.75 ± 0.03, Ω m = 0.29 ± 0.02, and σ 8 (Ω m /0.27) 0.3 = 0.764 ± 0.025. The value of σ 8 is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find σ 8 (Ω m /0.27) 0.3 = 0.78 ± 0.01 and a tighter one-dimensional range σ 8 = 0.77 ± 0.02. We find that the larger values of σ 8 and Ω m preferred by Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the ΛCDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make further progress in this field.
Automatic Detection-Extraction-Classification for a Large Number of Stellar Spectra from Slitless Wide Field Spectroscopy. A Project for AVO
ESO ASTROPHYSICS SYMPOSIA
ABSTRACT The distribution of spectral types in extended stellar systems in galaxies can be a powe... more ABSTRACT The distribution of spectral types in extended stellar systems in galaxies can be a powerful mine of information regarding: • 1. not only the properties of the stellar content (such as age, composition) but also • 2. the spatial distribution of certain types in order to trace specific structures (such as star forming regions and their geometry) Objective prism plates are ideal data for this analysis, since thousands of spectra have been reported simultaneously. Even more so, when using low dispersion prism plates we are dealing with a pool of stellar spectra. The full exploitation of digitized spectra in 1.2m UK Schmidt plates for a large number of stars involves three main automatic stages. • Detection of the spectra • Extraction of their images • Classification Automated methods for detection, extraction and classification published previously (Bratsolis et al. 1998, 2000a) have been implemented in a small SMC area very successfully.
Proceedings of CMB and Physics of the Early Universe — PoS(CMB2006), 2007
The Level 1 of the PLANCK Low Frequency Instrument (PLANCK/LFI) Data Processing Centre (DPC) is d... more The Level 1 of the PLANCK Low Frequency Instrument (PLANCK/LFI) Data Processing Centre (DPC) is devoted to the handling of scientific and housekeeping telemetry. It receives raw telemetry packets from the LFI through a tailored version of the ESA telemetry handling software SCOS 2000, and generates time ordered information of scientific and housekeeping data to be processed by the subsequent DPC levels. In addition, the Level 1 performs live diagnostics on the LFI telemetry. An end-to-end test has been performed recently at the LFI integration site (Alcatel Alenia Space, Milan) using the qualification model equipment of the on-board Data Acquisition Electronics and Data Processing unit, and its core software. For scientific data, the test is based on the injection of deterministic signals with known properties in the acquisition electronics and their comparison with the signal reconstructed from the telemetry data. A regression test has been performed on the housekeeping data by inserting known parameters values into a set of real housekeeping packets.
Stellar evolutionary models are a fundamental tool for addressing many astrophysical issues. For ... more Stellar evolutionary models are a fundamental tool for addressing many astrophysical issues. For such a reason, it is of fundamental relevance to make them available to the whole scientific community in an easy and direct way. We briefly review the main ingredients requested for computing stellar models and show some illustrative scientific cases concerning the comparison between model predictions and
Workflow and science gateway technologies have been adopted by scientific communities as a valuab... more Workflow and science gateway technologies have been adopted by scientific communities as a valuable tool to carry out complex experiments. They oer the possibility to perform computations for data analysis and simulations, whereas hiding details of the complex infrastructures underneath. In this paper we describe our experiences in creating workflows oriented science gateways based on gUSE/WS-PGRADE technology that allow to build user–friendly science gateways for Astronomers.
Modelling uncertainties at small scales, i.e. high k in the power spectrum P (k), due to baryonic... more Modelling uncertainties at small scales, i.e. high k in the power spectrum P (k), due to baryonic feedback, nonlinear structure growth and the fact that galaxies are biased tracers poses a significant obstacle to fully leverage the constraining power of the Euclid wide-field survey. k-cut cosmic shear has recently been proposed as a method to optimally remove sensitivity to these scales while preserving usable information. In this paper we generalise the k-cut cosmic shear formalism to 3 × 2 point statistics and estimate the loss of information for different k-cuts in a 3 × 2 point analysis of the Euclid data. Extending the Fisher matrix analysis of Euclid Collaboration: Blanchard et al. (2019), we assess the degradation in constraining power for different k-cuts. We find that taking a k-cut at 2.6 h Mpc −1 yields a dark energy Figure of Merit (FOM) of 1018. This is comparable to taking a weak lensing cut at = 5000 and a galaxy clustering and galaxy-galaxy lensing cut at = 3000 in a traditional 3 × 2 point analysis. We also find that the fraction of the observed galaxies used in the photometric clustering part of the analysis is one of the main drivers of the FOM. Removing 50% (90%) of the clustering galaxies decreases the FOM by 19% (62%). Given that the FOM depends so heavily on the fraction of galaxies used in the clustering analysis, extensive efforts should be made to handle the real-world systematics present when extending the analysis beyond the luminous red galaxy (LRG) sample.
Grid Data Source Engine: Grid gateway to the Virtual Observatory
… and Systems XV, 2006
... Baruffolo2, Fabio ~ Leopoldo Benacchio2 Istituto Nazioriale di Astrofisica, 00136 Rome, Italy... more ... Baruffolo2, Fabio ~ Leopoldo Benacchio2 Istituto Nazioriale di Astrofisica, 00136 Rome, ItalyEdgardo Ambrosi, Antonia ... Catalog and the the archive of observational data from the Italian Galileo National ... X, ed. FR Harnden, Jr., FA Primini, &amp;amp; HE Payne (San Francisco: ASP), 160 ...
The Euclid mission – with its spectroscopic galaxy survey covering a sky area over 15 000 deg2 in... more The Euclid mission – with its spectroscopic galaxy survey covering a sky area over 15 000 deg2 in the redshift range 0.9 < z < 1.8 – will provide a sample of tens of thousands of cosmic voids. This paper thoroughly explores for the first time the constraining power of the void size function on the properties of dark energy (DE) from a survey mock catalogue, the official Euclid Flagship simulation. We identified voids in the Flagship light-cone, which closely matches the features of the upcoming Euclid spectroscopic data set. We modelled the void size function considering a state-of-the art methodology: we relied on the volume-conserving (Vdn) model, a modification of the popular Sheth & van de Weygaert model for void number counts, extended by means of a linear function of the large-scale galaxy bias. We found an excellent agreement between model predictions and measured mock void number counts. We computed updated forecasts for the Euclid mission on DE from the void size func...
The large infrastructure projects for the next decade will allow a new quantum leap in terms of n... more The large infrastructure projects for the next decade will allow a new quantum leap in terms of new possible science. ESFRI, the European Strategy Forum on Research Infrastructures, a strategic initiative to develop the scientific integration of Europe, has identified four facilities (SKA, CTA, KM3Net and E-ELT) deserving priority in support. The ASTERICS project aims to address the cross-cutting synergies and common challenges shared by the various Astronomy ESFRI and other world-class facilities. The project (22 partners across Europe) is funded by the EU Horizon 2020 programme with 15 MEuro in 4 years. It brings together for the first time the astronomy, astrophysics and particle astrophysics communities, in addition to other related research infrastructures.
The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic ... more The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of i ∼ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage iv dark energy projects, particularly Euclid and the Nancy Grace Roman Space Telescope (Roman), which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B–2019B semesters using the DEIMOS, LRIS, and MOSFIRE multiobject spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 < z p < 2.6 range of interest for the Euclid cosmological goals, then with the current data release, C3R2 has increased t...
We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, upd... more We provide predictions of the yield of 7 < z < 9 quasars from the Euclid wide survey, updating the calculation presented in the Euclid Red Book in several ways. We account for revisions to the Euclid near-infrared filter wavelengths; we adopt steeper rates of decline of the quasar luminosity function (QLF; Φ) with redshift, Φ ∝ 10k(z − 6), k = −0.72, and a further steeper rate of decline, k = −0.92; we use better models of the contaminating populations (MLT dwarfs and compact early-type galaxies); and we make use of an improved Bayesian selection method, compared to the colour cuts used for the Red Book calculation, allowing the identification of fainter quasars, down to JAB ∼ 23. Quasars at z > 8 may be selected from Euclid OYJH photometry alone, but selection over the redshift interval 7 < z < 8 is greatly improved by the addition of z-band data from, e.g., Pan-STARRS and LSST. We calculate predicted quasar yields for the assumed values of the rate of decline o...
Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at ... more Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible
Proceedings of the International Astronomical Union, 2014
Euclid is the next ESA mission devoted to cosmology. It aims at observing most of the extragalact... more Euclid is the next ESA mission devoted to cosmology. It aims at observing most of the extragalactic sky, studying both gravitational lensing and clustering over ~15,000 square degrees. The mission is expected to be launched in year 2020 and to last six years. The sheer amount of data of different kinds, the variety of (un)known systematic effects and the complexity of measures require efforts both in sophisticated simulations and techniques of data analysis. We review the mission main characteristics, some aspects of the the survey and highlight some of the areas of interest to this meeting.
Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in... more Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization
Planck intermediate results. XXVI. Optical identification and redshifts of Planck clusters with t... more Planck intermediate results. XXVI. Optical identification and redshifts of Planck clusters with the RTT150 telescope
Publications of the Astronomical Society of the Pacific, 2008
In order to offer an intuitive but effective access to a growing number of cosmological simulatio... more In order to offer an intuitive but effective access to a growing number of cosmological simulations, we have developed the Italian Theoretical Virtual Observatory project (ITVO), as described by Pasian and colleagues in 2006. In this work we describe two Web portals as two ways to access and share complex data coming from numerical astrophysical simulations. We present a set of Web services aimed at offering services such as Simple Numeric Access (ProtocolSNAPSimple Numeric Access Protocol), as described by Gheller and colleagues in 2006, and Randomizers dealing with different data formats. The Web services technology allows us to run a particular task (a SNAP job, for instance) close to its data, avoiding an expensive data transfer.
Monthly Notices of the Royal Astronomical Society, 2010
QUICK DETECTION SYSTEM or QDS is a software package that has been developed for detecting point s... more QUICK DETECTION SYSTEM or QDS is a software package that has been developed for detecting point sources in the Planck satellite data as soon as the data become available, a few days after transmission to the Earth. Point sources are detected by filtering the data with a filter defined by the Mexican hat wavelet. An alert is generated on those detections that are found to be interesting, such as prominent flaring, according to the criteria specified to the software. The goal is to detect spectral or flux variability in active galactic nuclei so that instant multifrequency follow-up observations with other instruments could be arranged to study the interesting behaviour.
We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applyi... more We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 100 to 857 GHz frequency channel maps from the Planck survey. This map shows an obvious galaxy cluster tSZ signal that is well matched with blindly detected clusters in the Planck SZ catalogue. To characterize the signal in the tSZ map we have computed its angular power spectrum. At large angular scales (< 60), the major foreground contaminant is the diffuse thermal dust emission. At small angular scales (> 500) the clustered cosmic infrared background and residual point sources are the major contaminants. These foregrounds are carefully modelled and subtracted. We thus measure the tSZ power spectrum over angular scales 0.17 • < ∼ θ < ∼ 3.0 • that were previously unexplored. The measured tSZ power spectrum is consistent with that expected from the Planck catalogue of SZ sources, with clear evidence of additional signal from unresolved clusters and, potentially, diffuse warm baryons. Marginalized band-powers of the Planck tSZ power spectrum and the best-fit model are given. The non-Gaussianity of the Compton parameter map is further characterized by computing its 1D probability distribution function and its bispectrum. The measured tSZ power spectrum and high order statistics are used to place constraints on σ 8 .
We present constraints on cosmological parameters using number counts as a function of redshift f... more We present constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude σ 8 and matter density parameter Ω m in a flat ΛCDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that σ 8 = 0.75 ± 0.03, Ω m = 0.29 ± 0.02, and σ 8 (Ω m /0.27) 0.3 = 0.764 ± 0.025. The value of σ 8 is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find σ 8 (Ω m /0.27) 0.3 = 0.78 ± 0.01 and a tighter one-dimensional range σ 8 = 0.77 ± 0.02. We find that the larger values of σ 8 and Ω m preferred by Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the ΛCDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make further progress in this field.
Automatic Detection-Extraction-Classification for a Large Number of Stellar Spectra from Slitless Wide Field Spectroscopy. A Project for AVO
ESO ASTROPHYSICS SYMPOSIA
ABSTRACT The distribution of spectral types in extended stellar systems in galaxies can be a powe... more ABSTRACT The distribution of spectral types in extended stellar systems in galaxies can be a powerful mine of information regarding: • 1. not only the properties of the stellar content (such as age, composition) but also • 2. the spatial distribution of certain types in order to trace specific structures (such as star forming regions and their geometry) Objective prism plates are ideal data for this analysis, since thousands of spectra have been reported simultaneously. Even more so, when using low dispersion prism plates we are dealing with a pool of stellar spectra. The full exploitation of digitized spectra in 1.2m UK Schmidt plates for a large number of stars involves three main automatic stages. • Detection of the spectra • Extraction of their images • Classification Automated methods for detection, extraction and classification published previously (Bratsolis et al. 1998, 2000a) have been implemented in a small SMC area very successfully.
Proceedings of CMB and Physics of the Early Universe — PoS(CMB2006), 2007
The Level 1 of the PLANCK Low Frequency Instrument (PLANCK/LFI) Data Processing Centre (DPC) is d... more The Level 1 of the PLANCK Low Frequency Instrument (PLANCK/LFI) Data Processing Centre (DPC) is devoted to the handling of scientific and housekeeping telemetry. It receives raw telemetry packets from the LFI through a tailored version of the ESA telemetry handling software SCOS 2000, and generates time ordered information of scientific and housekeeping data to be processed by the subsequent DPC levels. In addition, the Level 1 performs live diagnostics on the LFI telemetry. An end-to-end test has been performed recently at the LFI integration site (Alcatel Alenia Space, Milan) using the qualification model equipment of the on-board Data Acquisition Electronics and Data Processing unit, and its core software. For scientific data, the test is based on the injection of deterministic signals with known properties in the acquisition electronics and their comparison with the signal reconstructed from the telemetry data. A regression test has been performed on the housekeeping data by inserting known parameters values into a set of real housekeeping packets.
Stellar evolutionary models are a fundamental tool for addressing many astrophysical issues. For ... more Stellar evolutionary models are a fundamental tool for addressing many astrophysical issues. For such a reason, it is of fundamental relevance to make them available to the whole scientific community in an easy and direct way. We briefly review the main ingredients requested for computing stellar models and show some illustrative scientific cases concerning the comparison between model predictions and
Workflow and science gateway technologies have been adopted by scientific communities as a valuab... more Workflow and science gateway technologies have been adopted by scientific communities as a valuable tool to carry out complex experiments. They oer the possibility to perform computations for data analysis and simulations, whereas hiding details of the complex infrastructures underneath. In this paper we describe our experiences in creating workflows oriented science gateways based on gUSE/WS-PGRADE technology that allow to build user–friendly science gateways for Astronomers.
Modelling uncertainties at small scales, i.e. high k in the power spectrum P (k), due to baryonic... more Modelling uncertainties at small scales, i.e. high k in the power spectrum P (k), due to baryonic feedback, nonlinear structure growth and the fact that galaxies are biased tracers poses a significant obstacle to fully leverage the constraining power of the Euclid wide-field survey. k-cut cosmic shear has recently been proposed as a method to optimally remove sensitivity to these scales while preserving usable information. In this paper we generalise the k-cut cosmic shear formalism to 3 × 2 point statistics and estimate the loss of information for different k-cuts in a 3 × 2 point analysis of the Euclid data. Extending the Fisher matrix analysis of Euclid Collaboration: Blanchard et al. (2019), we assess the degradation in constraining power for different k-cuts. We find that taking a k-cut at 2.6 h Mpc −1 yields a dark energy Figure of Merit (FOM) of 1018. This is comparable to taking a weak lensing cut at = 5000 and a galaxy clustering and galaxy-galaxy lensing cut at = 3000 in a traditional 3 × 2 point analysis. We also find that the fraction of the observed galaxies used in the photometric clustering part of the analysis is one of the main drivers of the FOM. Removing 50% (90%) of the clustering galaxies decreases the FOM by 19% (62%). Given that the FOM depends so heavily on the fraction of galaxies used in the clustering analysis, extensive efforts should be made to handle the real-world systematics present when extending the analysis beyond the luminous red galaxy (LRG) sample.
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Papers by Fabio Pasian