Simple Spectral Access Protocol Version 1.04

Tody, Doug; Dolensky, M.; McDowell, Jonathan; Bonnarel, F.; Budavàri, Tamás; Busko, I.; Micol, A.; Osuna, P.; Salgado, J.; Škoda, Petr; Thompson, Richard A.; Valdes, F.

doi:10.5479/ads/bib/2008ivoa.spec.0201d

Cited by 5 publications

(6 citation statements)

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“…Last, but not least, the IRAF implementation of rvsao did not allow a direct interface with the VIPGI package used for VVDS Data reduction (Scodeggio et al 2005). For all these reasons, we have decided to develop EZ (Easy redshift, pronounced "easy"), a new tool which inherits from the rvsao experience and the cross correlation technique, but allows to be easily plugged within VIPGI and could also be used as a VO-compliant tool via SSAP (Tody et al 2008) or other communication protocols. From the user's point of view, the most important requirement was to be able to run the program both in a completely unsupervised and in fully interactive mode, with a user friendly graphical interface to inspect the results obtained using different parameters or templates.…”

Section: Introductionmentioning

confidence: 99%

EZ: A Tool For Automatic Redshift Measurement

Garilli

Fumana

Franzetti

et al. 2010

PUBL ASTRON SOC PAC

117

118

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We present EZ (Easy redshift), a tool we have developed within the VVDS project to help in redshift measurement from otpical spectra. EZ has been designed with large spectroscopic surveys in mind, and in its development particular care has been given to the reliability of the results obtained in an automatic and unsupervised mode. Nevertheless, the possibility of running it interactively has been preserved, and a graphical user interface for results inspection has been designed. EZ has been successfully used within the VVDS project, as well as the zCosmos one. In this paper we describe its architecture and the algorithms used, and evaluate its performances both on simulated and real data. EZ is an open source program, freely downloadable from http://cosmos.iasf-milano.inaf.it/pandora.

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Section: Introductionmentioning

confidence: 99%

EZ: A Tool For Automatic Redshift Measurement

Garilli

Fumana

Franzetti

et al. 2010

PUBL ASTRON SOC PAC

117

118

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“…10 An analogue to SIAP, this protocol allows a client to ask an archive what spectra are available from a region on the sky, with a given spectral bandpass, or time of observation. The spectra could be static data products or generated on-the-fly based on the user input.…”

Section: Vo Standards: the Alphabet Soup For Archivesmentioning

confidence: 99%

Building archives in the virtual observatory era

et al. 2010

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Broad support for Virtual Observatory (VO) standards by astronomical archives is critical for the success of the VO as a research platform. Indeed, a number of effective data discovery, visualization, and integration tools have been created which rely on this broad support. Thus, to an archive, the motivation for supporting VO standards is strong. However, we are now seeing a growing trend among archive developers towards leveraging VO standards and technologies not just to provide interoperability with the VO, but also to support an archive's internal needs and the needs of the archive's primary user base. We examine the motivation for choosing VO technologies for implementing an archive's functionality and list several current examples, including from the Hubble Legacy Archive, NASA HEASARC, NOAO, and NRAO. We will also speculate on the effect that VO will have on some of the ambitious observatory projects planned for the near future.

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“…Bonifacio et al 2009, and references therein), and of carbon stars (e.g. Wahlin et al 2006) and AGB stars (García-Hernández et al 2007).…”

Section: Science With Pollux Datamentioning

confidence: 99%

“…5) or Aladin 9 . POLLUX is registered in the different registries 10 as a service using the Simple Spectra Access Protocol (SSAP, Tody et al 2008) and the Theoretical Spectra Access Protocol (TSAP). The SSAP defines a uniform interface to track and access 1-D spectra.…”

Section: Orientation Towards the Virtual Observatorymentioning

confidence: 99%

POLLUX: a database of synthetic stellar spectra

Palacios¹,

Gebran²,

Josselin³

et al. 2010

A&A

137

116

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Aims. Synthetic spectra are needed to determine fundamental stellar and wind parameters of all types of stars. They are also used for the construction of theoretical spectral libraries helpful for stellar population synthesis. Therefore, a database of theoretical spectra is required to allow rapid and quantitative comparisons to spectroscopic data. We provide such a database offering an unprecedented coverage of the entire Hertzsprung-Russell diagram. Methods. We present the POLLUX database of synthetic stellar spectra. For objects with T eff ≤ 6000 K, MARCS atmosphere models are computed and the program TURBOSPECTRUM provides the synthetic spectra. ATLAS12 models are computed for stars with 7000 K ≤ T eff ≤ 15 000 K. SYNSPEC gives the corresponding spectra. Finally, the code CMFGEN provides atmosphere models for the hottest stars (T eff > 25 000 K). Their spectra are computed with CMF_FLUX. Both high resolution (R > 150 000) optical spectra in the range 3000 to 12 000 Å and spectral energy distributions extending from the UV to near-IR ranges are presented. These spectra cover the HR diagram at solar metallicity. Results. We propose a wide variety of synthetic spectra for various types of stars in a format that is compliant with the Virtual Observatory standards. A user-friendly web interface allows an easy selection of spectra and data retrieval. Upcoming developments will include an extension to a large range of metallicities and to the near-IR high resolution spectra, as well as a better coverage of the HR diagram, with the inclusion of models for Wolf-Rayet stars and large datasets for cool stars. The POLLUX database is accessible at http://pollux.graal.univ-montp2.fr/ and through the Virtual Observatory.Key words. astronomical databases: miscellaneous -stars: general -techniques: spectroscopic Presentation and aim of the databasePOLLUX is a database of synthetic stellar spectra developed at the GRAAL laboratory (Université Montpellier II -CNRS). Its aim is to provide a comprehensive library of theoretical stellar spectra with a broad coverage of the atmospheric parameters (effective temperature T eff , gravity log g and metallicity [Fe/H]). Both high resolution optical spectra and spectral energy distributions are provided for O to M stars.POLLUX spectra are expected to be useful to astrophysicists for stellar or (extra-)galactic applications in several respects: accurate determination of fundamental properties of stars, abundance determinations, radial velocities and stellar dynamics, tests of the current state-of-the-art model atmospheres, stellar population synthesis. POLLUX spectra can also be used for teaching purposes oriented toward spectroscopy and model atmospheres.In a framework where various grids of model atmospheres, SEDs and synthetic spectra computed with the MARCS 1 , ATLAS9 2 and CMFGEN 3 codes respectively are available on Copy of database is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-b...

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Simple Spectral Access Protocol Version 1.04

Cited by 5 publications

References 0 publications

EZ: A Tool For Automatic Redshift Measurement

EZ: A Tool For Automatic Redshift Measurement

Building archives in the virtual observatory era

POLLUX: a database of synthetic stellar spectra

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