Surface brightness fluctuation spectrum: a new probe of evolved stars in unresolved stellar populations

被引：8

作者：

Mitzkus, Martin ^{[1
]}

Walcher, C. Jakob ^{[1
]}

Roth, Martin M. ^{[1
]}

Coelho, Paula R. T. ^{[2
]}

Cioni, Maria-Rosa L. ^{[1
]}

Raimondo, Gabriella ^{[3
]}

Rejkuba, Marina ^{[4
]}

机构：

[1] Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany

[2] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, R Matao 1226, BR-05508090 Sao Paulo, Brazil

[3] INAF Osservatorio Astron Abruzzo, Via Mentore Maggini Snc, I-64100 Teramo, Italy

[4] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 480卷 / 01期

基金：

欧洲研究理事会;

关键词：

methods: data analysis; galaxies: elliptical and lenticular; cD-galaxies: individual: NGC 5102; galaxies: stellar content; EARLY-TYPE GALAXIES; NEWTON-TELESCOPE LIBRARY; EVOLUTIONARY SYNTHESIS; EMPIRICAL CALIBRATION; SYNTHETIC PHOTOMETRY; DISTANCE INDICATOR; MODEL ATMOSPHERES; GLOBULAR-CLUSTERS; BRANCH STARS; SCALED-SOLAR;

D O I：

10.1093/mnras/sty1840

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The surface brightness fluctuation (SBF) method measures spatial fluctuations due to the most luminous stars in a galaxy. Besides being useful for distance measurements, it also provides diagnostic power to investigate the contribution of the brightest stars to the underlying unresolved stellar population. We apply the SBF technique to every wavelength layer in integral field spectroscopy data obtained with the MUSE instrument. This yields the first SBF spectrum of a galaxy. SBF spectra combine the sensitivity of SBF to luminous stars with the physical information content of spectra. We show that the SBF spectrum of the S0 galaxy NGC 5102 is dominated by spectra of M-type giants (red giant branch, asymptotic giant branch, and red supergiant stars). We build the first stellar population synthesis tool that predicts SBF spectra. Through comparison of integrated spectra from our new tool with published model spectra, we confirm that it is mathematically correct. We use the integrated spectrum and a bootstrap method to derive an ensemble of (degenerate) star formation histories of NGC 5102. We compute a model SBF spectrum for each star formation history. Given that some models do not reproduce the observed SBF spectrum well, we are able to obtain additional constraints on the star formation history, leading to marginally reduced uncertainties on the mean age and metallicity. This result is confirmed by modelling mock spectra with different star formation histories.

引用

页码：629 / 651

页数：23

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