Astro+ database. I. Description and first results

Abstract

The vast amounts of spectroscopic data for massive stars provided by previous and existing instruments on ground-based and space-based telescopes have saturated our capability to process them by human inspection routines. Consequently, there is a pressing need for fully automatic machine-assisted tools to help handle incoming data. To this end, we present the development of a massive star spectroscopic interactive database, Astro+. We aim to provide users with a reliable, versatile, and user-friendly platform that will be significant for understanding massive stars and set an important precedent for future open-access astrophysical research. This tool allows authorized users to upload their own spectra and by using the fully automated tool HiLineThere, a Python-based program, it can homogeneously derive basic stellar parameters, such as v_ rad , v , and łog , g for massive OB-type stars, using a solar-metallicity grid of FASTWIND models, and i, T_ eff rad , $ Fe/H $, T_ eff , and łog , g for red supergiant stars, in a completely autonomous way. Here we present the first results of the tool HiLineThere on optical spectra for OB-type and red supergiants. We compare the output of our analysis for OB-type stars with literature values for a large sample of well-studied objects, finding differences within the expected error ranges: T_ eff ∼ 800,K, łog g ∼ 0.1,dex, and v i ∼ 10,km,s-1. Preliminary tests on early-B stars also show consistent results during the transition to lower temperatures. For red supergiants, we find differences within 7$,km,s^-1 in v_ rad and ∼ 300,K in $T_ eff for two test samples.