| dc.creator | EMANUELE BERTONE TARICCO | |
| dc.creator | MIGUEL Y ROSA MARIA CHAVEZ DAGOSTINO | |
| dc.creator | LINO HECTOR RODRIGUEZ MERINO | |
| dc.date | 2008 | |
| dc.date.accessioned | 2023-07-25T16:22:51Z | |
| dc.date.available | 2023-07-25T16:22:51Z | |
| dc.identifier | http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/1033 | |
| dc.identifier.uri | https://repositorioslatinoamericanos.uchile.cl/handle/2250/7806232 | |
| dc.description | Aims. The fast improvement of spectroscopic observations makes mandatory a strong effort on the theoretical side to better reproduce the spectral energy distribution (SED) of stars at high spectral resolution. In this regard, relying on the Kurucz Atlas/Synthe original codes we computed the Bluered library, consisting of 832 synthetic SED of stars, that cover a large parameter space at very high spectral resolution (R = 500 000) along the 3500−7000 Å wavelength range. Methods. Bluered synthetic spectra have been used to assess in finer detail the intrinsic reliability and the performance limits of the Atlas theoretical framework. The continuum-normalized spectra of the Sun, Arcturus, and Vega, plus a selected list of 45 bright stars with high-quality SEDs from the Prugniel & Soubiran Elodie catalog, form our sample designed to probe the global properties of synthetic spectra across the entire range of H-R parameters. Results. Atlas models display a better fitting performance with increasing stellar temperature. High-resolution spectra of Vega, the Sun, and Arcturus have been reproduced at R = 100 000, respectively, within a 0.7%, 4.5%, and 8.8% relative scatter in residual flux. In all the three cases, the residual flux distribution shows a significant asymmetry (skewness parameter γ = −2.21, −0.98, −0.67, respectively), which neatly confirms an overall “excess” of theoretical line blanketing. For the Sun, this apparent discrepancy is alleviated, but not recovered, by a systematic decrease (−40%) of the line oscillator strengths, log(ɡf ), especially referring to iron transitions. Definitely, a straight “astrophysical” determination of log(ɡf) for each individual atomic transition has to be devised to overcome the problem. By neglecting overblanketing effects in theoretical models when fitting high-resolution continuum-normalized spectra of real stars, we lead to a systematically warmer effective temperature (between +80 and +300 K for the solar fit) and a slightly poorer metal content. | |
| dc.format | application/pdf | |
| dc.language | eng | |
| dc.publisher | Astronomy and Astrophysics | |
| dc.relation | citation:Bertone, E., et al., (2008). Probing atlas model atmospheres at high spectral resolution stellar synthesis and reference template validation, Astronomy and Astrophysics, Vol.485(3):823-835 | |
| dc.rights | info:eu-repo/semantics/openAccess | |
| dc.rights | http://creativecommons.org/licenses/by-nc-nd/4.0 | |
| dc.subject | info:eu-repo/classification/cti/1 | |
| dc.subject | info:eu-repo/classification/cti/21 | |
| dc.subject | info:eu-repo/classification/cti/21 | |
| dc.title | Probing atlas model atmospheres at high spectral resolution. Stellar synthesis and reference template validation | |
| dc.type | info:eu-repo/semantics/article | |
| dc.type | info:eu-repo/semantics/acceptedVersion | |
| dc.audience | students | |
| dc.audience | researchers | |
| dc.audience | generalPublic | |
