ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Astronomical Spectroscopy in the VO era: VOSpec Pedro Osuna Isa Barbarisi, Jesus Salgado, Andrea Laruelo European Space Astronomy Centre (ESAC) Science Archives and VO Team

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Making data available in the Internet Create document WEB SERVER robots

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Making data available in the VO Create service SSA SERVER

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Making data available in VO: DAL Toolkit Config Files Spectra FITS Files Ingestor DB Server DAL Request VOTable File Sys

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC VOSpec Main Features Handle SSAP spectra Open local Spectra (Fits or VOTable) Create a SED of spectra coming from a wide range of different providers registered in the VO Registry ( and also coming from local data Create SSAP Wrapper with your own set of local spectra and immediately display it Graphic options like color modification, zoom, unzoom, change spectra visualization, change units etc.. Save results as Image/VOTable Math operations like Polynomial, BlackBody fitting, Gaussian, Nomalization, DeReddening, Red-shift, Luminosity Differences etc. Access to Theoretical Spectra through TSAP and Spectral Atomic Lines through SLAP Interoperability with other vo-aware tools through Plastic Technology

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC De-Reddening Interstellar reddening is a phenomenon associated with interstellar extinction where the spectrum of electromagnetic radiation from a radiation source changes characteristics from that which was emitted. Reddening occurs due to the light scattering off dust and other matter in the interstellar medium. It preferentially removes shorter wavelength photons from a radiated spectrum while leaving behind the longer wavelength photons (in the optical, light that is redder), leaving the spectroscopic lines unchanged VOSpec povides support to this phenomenon allowing to apply the Calzetti, Cardelli O’Donnel or LMC formula, depending by the case. Please visit the VOSpec User Manual to see the video of the De-Reddening functionality.

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC De-Reddening – IRAS case

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Theoretical Spectra Access in VOSpec VOSpec allows the user to rescale theoretical spectra using real spectral data for the object to be studied. Even if there are many differences between theoretical and real spectra, it’s been studied a solution to unify them in a common access protocol in order to visualize them in the same plot Main differences between both kind of spectra are the following: - Models have specific input parameters - Theoretical Spectra are not normalized

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Simple Line Access through VOSpec There is a scientific need to have access to spectral line databases in the VO. Many science cases could make use of this kind of access VOSpec provides access to Atomic Line Databases through the Simple Line Access Protocol (SLAP) Please visit the VOSpec User Manual to see the video of the SLAP functionality.

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Best Fit fitting tool MOTIVATION Currently, to find the model that best fits a given SED: Choose parameters manually Inspect result visually (“Chi-by-eye”) Modify parameters manually Reinspect visually Loop… GOAL Best Fit finds the best fit model automatically METHOD Levenberg-Marquardt Chi-square minimization algorithm

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Best Fit step by step  Selecting TSA server Initial model Best fit model minimization proccess Select TSA server Select initial parameters

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Plastic Technology and Applications PLASTIC is a protocol for communication between client-side astronomy applications. Through PLASTIC applications can do tasks such as instruct each other to load Spectra, VOTables, highlight a subset of rows or load an image of a particular area of sky. Although such operations are quite simple, they enable powerful collaborations between tools. The philosophy is that the astronomer should have a suite of interoperating tools at his disposal, each of which does one thing well and which can be composed according to his particular needs. VOSpec allows registration to the Plastic Hub and it can interoperate with other VO-aware tools like Aladin, Astroscope, VOQuest etc Please visit for more details about the projecthttp://plastic.sourceforge.net Sending spectra from Astroscope to VOSpec through Plastic Sending spectra from Aladin to VOSpec through Plastic

ESAVO/European Space Astronomy Centre (ESAC) Villafranca del Castillo, MADRID (SPAIN) Pedro Osuna ASVOWS Mar 2007 ESAC Future implementations on VOSpec You name it, we implement it. See VOSpec at work: And the User Manual at: