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YBC: a Stellar Bolometric Corrections Database with Variable Extinction Coefficients

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YBC: a Stellar Bolometric Corrections Database with Variable Extinction Coefficients A&A 632, A105 (2019) Astronomy https://doi.org/10.1051/0004-6361/201936612 & c ESO 2019 Astrophysics YBC: a stellar bolometric corrections database with variable extinction coefficients Application to PARSEC isochrones? Yang Chen (H洋)1, Léo Girardi2, Xiaoting Fu (&Sw)3, Alessandro Bressan4, Bernhard Aringer1, Piero Dal Tio1,2, Giada Pastorelli1, Paola Marigo1, Guglielmo Costa4, and Xing Zhang ( 星)5 1 Dipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy e-mail: [email protected] 2 Osservatorio Astronomico di Padova – INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 3 The Kavli Institute for Astronomy and Astrophysics at Peking University, Beijing, PR China e-mail: [email protected] 4 SISSA, Via Bonomea 365, 34136 Trieste, Italy 5 Department of Astronomy, University of Science and Technology of China, Chinese Academy of Sciences, Hefei, Anhui 230026, PR China Received 1 September 2019 / Accepted 17 October 2019 ABSTRACT We present the YBC database of stellar bolometric corrections, in which we homogenise widely used theoretical stellar spectral libraries and provide BCs for many popular photometric systems, including Gaia filters. The database can easily be extended to additional photometric systems and stellar spectral libraries. The web interface allows users to transform their catalogue of theoretical stellar parameters into magnitudes and colours of selected filter sets. The BC tables can be downloaded or implemented into large simulation projects using the interpolation code provided with the database. We computed extinction coefficients on a star-by-star basis, hence taking into account the effects of spectral type and non-linearity dependency on the total extinction. We illustrate the use of these BCs in PARSEC isochrones. We show that using spectral-type dependent extinction coefficients is necessary for Gaia filters whenever AV & 0:5 mag. Bolometric correction tables for rotating stars and tables of limb-darkening coefficients are also provided. Key words. Hertzsprung-Russell and C-M diagrams – astronomical databases: miscellaneous – dust, extinction – open clusters and associations: individual: NGC 2425 – open clusters and associations: individual: Mellotte 22 1. Introduction therein). These libraries, which have different solar abundances, offer large grids of models covering different stellar parameters Bolometric corrections (BCs) are usually applied to the abso- (metallicity, Teff, and log g). However, currently there is a lack lute magnitude of a star to obtain its bolometric absolute mag- of a single, homogeneous, public database to synthesise these nitude or luminosity, or conversely, to predict the magnitudes libraries and provide BC tables for a large set of photometric of a model star in a given set of filters. Most modern versions of systems. BCs are usually based on theoretical stellar spectral libraries; see One of the obvious advantages of having a homogeneous for example Girardi et al.(2002), Casagrande & VandenBerg database for BCs would be to facilitate the comparison between (2014, 2018a). In some cases empirical stellar spectral libraries stellar models and the observations. Indeed, besides the differ- are also used for this purpose, however, they require addi- ences in the theoretical quantities such as log L=L and Teff tional calibration from theoretical atmosphere models and are of various stellar models, additional deviations are often intro- always limited by the coverage of stellar spectral type and duced from different authors using different BC tables. The pos- wavelength range (Sánchez-Blázquez et al. 2006; Rayner et al. sibility of testing the difference from those originally applied 2009; Chen et al. 2014a). In practice, BCs are often provided will become more critical with forthcoming facilities provid- along with, or can be easily computed from, spectral libraries ing photometry of much higher precision. This is especially obtained from the modelling of stellar atmospheres. Currently, true considering, for instance, the ∼10−4 mag errors expected the widely used theoretical stellar spectral libraries include for Gaia sources with G < 12 mag and >100 CCD transits, ATLAS9 (Castelli & Kurucz 2003) and PHOENIX (Allard et al. for a nominal mission with perfect calibrations (see Fig. 9 2012) for generic types of stars, MARCS (Gustafsson et al. in Evans et al. 2018), and the systematic errors smaller than COMARCS 2008) for cool or intermediate temperature stars, for 0.005 mag planned for Large Synoptic Survey Telescope (LSST) PoWR K/M/S/C stars (Aringer et al. 2009, 2016, 2019), and for single visits (Ivezic´ et al. 2019). It is also important to consider Wolf-Rayet (WR) stars (Gräfener et al. 2002, and references the different ways of handling the interstellar extinction in the ? The YBC database of stellar bolometric corrections is available at models, which is especially crucial when using either UV fil- http://stev.oapd.inaf.it/YBC ters (as in GALEX) or very broad passbands (such as the Gaia, Article published by EDP Sciences A105, page 1 of 13 A&A 632, A105 (2019) 21:1 −1 −2 −1 TESS, and HST/WFC3/UVIS extremely wide filters). In these 10 −2:5 erg s cm Å . The reference magnitudes thus are set to cases, fixed extinction coefficients are no longer valid and the −21.10 mag. effect of stellar spectral types becomes critical (Girardi et al. – Gunn systems (Thuan & Gunn 1976). In these systems, F- 2008). type subdwarfs, in particular BD +17 4708, are taken as the ref- In this work, we build a database in which we assemble erence stars instead of Vega. existing popular stellar spectral libraries to compute BC tables Among these, the Vega and AB magnitude systems are the homogeneously for a wide variety of photometric systems. The most widely adopted ones. At http://stev.oapd.inaf.it/ web interface of this database provides a convenient way for the cmd/photsys.html, the reader can check the information about users to transform their theoretical stellar catalogues into mag- the photometric systems supported. nitudes and colours, and hence to compare these samples with Usually, synthetic spectral libraries provide the stellar flux observations. This database has the flexibility to choose differ- at the stellar radius R. This flux Fλ is related to the effective ent stellar spectral libraries, thus allowing their differences to be temperature Teff of the star by easily investigated. The extinction coefficients have been com- Z 1 puted on a star-by-star basis, therefore the variation with spectral 4 Fbol ≡ Fλdλ = σTeff; (3) type has been taken into account. The non-linearity as a func- 0 tion of AV is included, which is important for highly attenuated targets. In this paper, we introduce the definitions of the BCs where σ is the Stefan–Boltzmann constant. By placing the star in Sect.2, the available stellar spectral libraries in Sect.3, and at 10 pc from the earth, the flux we receive is our C/Python code package in Sect.4. We compare some of our !2 results with the literature in Sect.5. In Sect.6, we discuss the R f = F 10−0:4Aλ ; spectral type dependent extinction coefficients. Section7 sum- λ,10 pc 10 pc λ marises the main results. where Aλ is the assumed extinction between the star and the 2. Bolometric corrections observer. Therefore, the absolute magnitude Mi for a photon- counting photometric system is In this section, we recall some basic relations concerning the BC, which are necessary for the discussion. Kurucz(1979), 2R λ2 3 6 λ fλ,10 pcS λ,idλ7 Bessell et al.(1998), and Girardi et al.(2002) provide a more − 6 λ1 7 Mi = 2:5log 6 R λ 7 + mi;0 exhaustive discussion. 46 2 0 57 λ fλ S λ,idλ First, we recall the definition of magnitude. Assuming we (at λ1 2 R λ 3 !2 2 −0:4Aλ earth) receive a radiation flux fλ (or fν) from a source, the mag- 6 R λFλ10 S λ,idλ7 6 λ1 7 nitude in a certain filter band i with transmission curve S λ,i is = −2:5log 6 7 + mi;0: (4) 46 10 pc R λ2 0 57 λ fλ S λ,idλ 2 R λ2 3 λ1 6 λ fλS λ,idλ 7 6 λ1 7 mi = −2:5log 6 7 + mi;0: (1) The definition of bolometric magnitude M is 46R λ2 0 57 bol λ f S λ,idλ λ1 λ Mbol = Mbol; − 2:5log(L=L ) In this equation, f 0 is the flux of the reference spectrum and m λ i;0 2 is the corresponding reference magnitude. These two quantities = Mbol; − 2:5log(4πR Fbol=L ): (5) depend on the photometric system and are discussed later. The According to the IAU 2015 resolution (Mamajek et al. 2015), the quantities λ1 and λ2 denote the lower and upper wavelength lim- its of the filter transmission curve, respectively. The above equa- absolute bolometric magnitude for the nominal solar luminosity 26 tion is valid for present-day photon-counting devices (CCDs or (3:828 × 10 W) is Mbol; = 4:74 mag. IR arrays). For more traditional energy-integrating systems the Given an absolute magnitude Mi in a given filter band i for a above equation should be changed to star of absolute bolometric magnitude Mbol, the bolometric cor- rection BCi is: 2 R λ2 3 6 fλS λ,idλ 7 6 λ1 7 mi = −2:5log 6 7 + mi;0: (2) BCi = Mbol − Mi: (6) 46R λ2 0 57 λ fλ S λ,idλ 1 By combing Eqs. (4)–(6), we have 0 0 Depending on the reference spectra fλ (or fν ), commonly 2 ! used magnitude systems are: 4πσ(10 pc) 4 – Vega magnitude systems. The spectrum of Vega (α Lyr) BCi = Mbol; − 2:5log − 2:5log(Teff) L is used as the reference spectrum.
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