sp_aceivo://org.gavo.dc/sp_ace/q/cThe GAVO DC teamBoeche, C.Demleitner, M.Heinl, H.2015-11-302016-02-042016-07-282017-06-212017-12-042019-08-122020-07-17GAVO Data Centre Team

Mönchhofstrasse 12-14, D-69120 Heidelberg

gavo@ari.uni-heidelberg.de+49 6221 54 1837stellar-abundancesspectroscopystellar-atmospheresastronomy-data-analysis SP_ACE computes stellar parameters (gravity, temperature) and element abundances from optical stellar spectra (`sample spectrum`_). It employs 1D stellar atmosphere models in Local Thermodynamic Equilibrium (LTE). The present service does not offer all the options available for SP_Ace as documented in `the tutorial`_. All options are available if running SP_Ace locally (cf. `download page`_). This service exposes an updated version containing some bug fixes with respect to the one described in the paper. .. _the tutorial: http://dc.g-vo.org/sp_ace/q/dist/static/tutorial.pdf .. _download page: http://dc.g-vo.org/sp_ace/q/dist/static .. _sample spectrum: http://dc.g-vo.org/sp_ace/q/c/static/fast_spectrum.txt2016A&A...587A...2Bhttp://dc.g-vo.org/sp_ace/q/c/info If you use results obtained by this service, please cite the original publication (see source meta) and acknowlege: This work has made use of the sp_ace spectral analysis tool version 1.4.http://dc.g-vo.org/SP_ACEhttps://dc.g-vo.org/SP_ACEhttp://dc.g-vo.org/sp_ace/q/c/api?https://dc.g-vo.org/sp_ace/q/c/api?GETapplication/x-votable+xmlUPLOADAn upload of the form 'spectrum,URL'; the input for this parameter is then taken from URL, which may be param:name for pulling the content from the inline upload name. Purpose of the upload: ASCII file with two columns: wavelength (in Angstrom) and continuum normalized flux. The spectrum must be radial velocity corrected (wavelengths in rest frame). The spectral resolution power should be between 2000 and 20000. SP_Ace handles spectra in the stellar parameters intervals Teff=[3600,7400]K, logg=[0.2,5.0], [M/H]=[-2.4,0.4]dex.charfwhmStarting value for estimation of FWHM of the instrument line profile.Angstromspect.line.width;instrrealwave_limsGive up to five wavelength intervals you want to analyze, starting from the lowest. Intervals not covered by the library will be ignored. The default setting is the range of wavelenghts currently processed by the software.chartforceForce solver to assume this temperature. Leave empty to let SP_Ace estimate this parameter.Kstat.param;phys;temperature.effectiverealgforceForce solver to assume this gravity. Leave empty to let SP_Ace estimate this parameter.stat.param;phys.gravityrealsnrforceForce solver to assume this signal to noise ratio on every pixel. Suggestion: Leave empty to let SP_Ace to estimate this parameter pixel-by-pixel.stat.param;stat.snrrealrv_iniProvide an estimation of the object's radial velocity in case the spectrum is not RV-corrected.km/sspect.dopplerVelocrealcompute_errorsMake SP_Ace estimate errors (this increases runtime significantly).charalphaIf selected, the output will only contain two abundances: 'alphas' and 'metals', which are the estimation of the abundances of alpha-process elements and non-alpha-process elements as if they were one element. Hint: This option is mostly useful with low-resolution (R ~ 2000) spectra. See the tutorial for more details.charno_normProcess the spectrum with the normalization provided by the user? This option switches off the internal re-normalization done by SP_Ace. Suggestion: Do not set unless you are absolutely sure that your normalization is right.charnorm_radThis parameter determines the flexibility of the curve used to fit the continuum during the re-normalization of the spectrum. The higher the number the more rigid the curve is (see discussion in the tutorial and in Sec.7.4 of the paper). Suggestion: leave the default value unless you know very well what you are doing.realabd_loopSwitch on the loop that iteratively derives stellar parameters (Teff, log g, [M/H]) and chemical abundances. Suggestion: do not set (see Sec. 8.5.1 of the paper). If your spectrum has low resolution (R ~ 2000), see discussion in the tutorial.charresponseformatFile format requested for output.meta.code.mimecharmaxrecMaximum number of records returned. Pass 0 to retrieve service parameters.integerverbExhaustiveness of column selection. VERB=1 only returns the most important columns, VERB=2 selects the columns deemed useful to the average user, VERB=3 returns a table with all available columns.integerhttp://dc.g-vo.org/sp_ace/q/c/capabilitieshttps://dc.g-vo.org/sp_ace/q/c/capabilitieshttp://dc.g-vo.org/sp_ace/q/c/availabilityhttps://dc.g-vo.org/sp_ace/q/c/availabilityhttp://dc.g-vo.org/sp_ace/q/c/tableMetadatahttps://dc.g-vo.org/sp_ace/q/c/tableMetadatasp_ace SP_ACE computes stellar parameters (gravity, temperature) and element abundances from optical stellar spectra (`sample spectrum`_). It employs 1D stellar atmosphere models in Local Thermodynamic Equilibrium (LTE). The present service does not offer all the options available for SP_Ace as documented in `the tutorial`_. All options are available if running SP_Ace locally (cf. `download page`_). This service exposes an updated version containing some bug fixes with respect to the one described in the paper. .. _the tutorial: http://dc.g-vo.org/sp_ace/q/dist/static/tutorial.pdf .. _download page: http://dc.g-vo.org/sp_ace/q/dist/static .. _sample spectrum: http://dc.g-vo.org/sp_ace/q/c/static/fast_spectrum.txtoutputelementElement symbolphys.atmol.elementcharnullableabElement abundance, logarithm of particle number relative to 1e12 H particles.phys.abundfloatnullableab_lowLower limit of 68% confidence interval of element abundancephys.abundfloatnullableab_upUpper limit of 68% confidence interval of element abundancephys.abundfloatnullablenlinesNumber of lines evaluated for this element.stat.fit.paramint