Age and Mass Constraints for a Young Massive Cluster in M31 Based on Spectral Energy Distribution Fitting

Ma, Jun; Wang, Song; Wu, Zhenyu; Zhang, Fan; Yang, Yanbin; Zhang, Tianmeng; Wu, Jianghua; Zhou, Xu; Jiang, Zhaoji; Chen, Jiansheng

doi:10.1088/0004-6256/141/3/86

Cited by 9 publications

(4 citation statements)

References 91 publications

(174 reference statements)

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“…In Fig. 14, we compare our ages with those in the literature, Beasley et al (2004), Perina et al (2010), Puzia et al (2005), Vansevičius et al (2009), Caldwell et al (2009Caldwell et al ( , 2011, Colucci et al (2009), Colucci et al (2014), Ma et al (2009Ma et al ( , 2011, Ma (2012), Wang et al (2010), Fan et al (2010), Kang et al (2012) and Cezario et al (2013). Beasley et al (2004) derive ages of 30 clusters in M31 from spectral indices.…”

Section: Comparison With Previous Age Estimatesmentioning

confidence: 99%

“…The comparison shows that our estimates are consistent with results from high-resolution spectroscopy. Ma et al (2009Ma et al ( , 2011; Wang et al (2010) and Fan et al (2010) estimate ages of M31 star clusters by SED fitting of multi-band 2009), Caldwell et al (2009Caldwell et al ( , 2011, Colucci et al (2009), Colucci et al (2014), Ma et al (2009Ma et al ( , 2011, Ma (2012), Wang et al (2010), Fan et al (2010), Kang et al (2012) and Cezario et al (2013). Our ages derived from full spectral fitting using PEGASE-HR SSP models for old clusters are plotted in black and those from SED fitting for young clusters are plotted in red.…”

Section: Comparison With Previous Age Estimatesmentioning

confidence: 99%

“…Figure14. Comparisons of ages from our analysis and those in the literature:Beasley et al (2004),Perina et al (2010),Puzia et al (2005),Vansevičius et al (2009),Caldwell et al (2009Caldwell et al ( , 2011,Colucci et al (2009),Colucci et al (2014),Ma et al (2009Ma et al ( , 2011,Ma (2012),Wang et al (2010),Fan et al (2010),Kang et al (2012) andCezario et al (2013). Our ages derived from full spectral fitting using PEGASE-HR SSP models for old clusters are plotted in black and those from SED fitting for young clusters are plotted in red.…”

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confidence: 95%

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The Lamost Spectroscopic Survey of Star Clusters in M31. Ii. Metallicities, Ages, and Masses

Chen¹,

Liu²,

Xiang³

et al. 2016

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We select from Paper I a sample of 306 massive star clusters observed with the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST) in the vicinity fields of M31 and M33 and determine their metallicities, ages and masses. Metallicities and ages are estimated by fitting the observed integrated spectra with stellar synthesis population (SSP) models with a pixel-to-pixel spectral fitting technique. Ages for most young clusters are also derived by fitting the multi-band photometric measurements with model spectral energy distributions (SEDs). The estimated cluster ages span a wide range, from several million years to the age of the universe. The numbers of clusters younger and older than 1 Gyr are respectively 46 and 260. With ages and metallicities determined, cluster masses are then estimated by comparing the multi-band photometric measurements with SSP model SEDs. The derived masses range from ∼ 10 3 to ∼ 10 7 M ⊙ , peaking at ∼ 10 4.3 and ∼ 10 5.7 M ⊙ for young (< 1 Gyr) and old (> 1 Gyr) clusters, respectively. Our estimated metallicities, ages and masses are in good agreement with available literature values. Old clusters richer than [Fe/H] ∼ −0.7 dex have a wide range of ages. Those poorer than [Fe/H] ∼ −0.7 dex seem to be composed of two groups, as previously found for Galactic GCs -one of the oldest ages with all values of metallicity down to ∼ −2 dex and another with metallicity increasing with decreasing age. The old clusters in the inner disk of M 31 (0 -30 kpc) show a clear metallicity gradient measured at −0.038 ± 0.023 dex/kpc.

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Section: Comparison With Previous Age Estimatesmentioning

confidence: 99%

Section: Comparison With Previous Age Estimatesmentioning

confidence: 99%

mentioning

confidence: 95%

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The Lamost Spectroscopic Survey of Star Clusters in M31. Ii. Metallicities, Ages, and Masses

Chen¹,

Liu²,

Xiang³

et al. 2016

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“…Mochejska et al 1998;Barmby & Huchra 2001;Kim et al 2007). In addition, a number of papers by Ma's group have been published on the M31 globular clusters (Fan et al 2006(Fan et al , 2008(Fan et al , 2009Jiang et al 2003;Ma et al 2006aMa et al ,b, 2007Ma et al , 2009bMa et al ,a, 2010Ma et al , 2011Ma 2011;Wang et al 2010), including the integrated magnitudes, colors, ages, masses, metallicities and structural parameters.…”

Section: Introductionmentioning

confidence: 99%

2MASS photometry and age estimation of the globular clusters in the outer halo of M31

Ma¹

2012

Res. Astron. Astrophys.

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We present the first photometric results in J, H, and K s from 2MASS imaging of 10 classical globular clusters in the far outer regions of M31. Combined with the V and I photometric data from previous literature, we constructed the color-color diagram between J − K s and V − I. By comparing the integrated photometric measurements with evolutionary models, we estimate the ages of these clusters. The results showed that, all of these clusters are older than 3 × 10 9 yrs, of which 4 are older than 10 Gyrs and the other 6 are in intermediate ages between 3 − 8 Gyrs. The masses for these outer halo GCs are from 7.0 × 10 4 M ⊙ to 1.02 × 10 6 M ⊙ . We argued that, GC2 and GC3, the ages, metallicities and the distance moduli of which are nearly the same, were accreted from the same satellite galaxy, if they did not form in situ. The statistical results show that, ages and metallicities for these 10 M31 outer halo GCs do not vary with projected radial position, and the relationship between age and metallicity doest not exit.

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The effects of the WISE/GALEX photometry for the SED-fitting with M31 star clusters and candidates

Zhang¹,

Wang²

2017

Astrophys Space Sci

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Spectral energy distribution (SED) fitting of stellar population synthesis models is an important and popular way to constrain the physical parameters -e.g., the ages, metallicities, masses for stellar population analysis. The previous works suggest that both blue-bands and red-bands photometry works for the SEDfitting. Either blue-domained or red-domained SED-fitting usually lead to the unreliable or biased results. Meanwhile, it seems that extending the wavelength coverage could be helpful. Since the Galaxy Evolution Explorer (GALEX) and Wide-field Infrared Survey Explorer (WISE) provide the FUV/NUV and midinfrared W 1/W 2 band data, we extend the SED-fitting to a wider wavelength coverage. In our work, we analyzed the effect of adding the FUV/NUV and W 1/W 2 band to the optical and near-infrared UBV RIJHK bands for the fitting with the Bruzual & Charlot 2003 (BC03) models and galev models. It is found that the FUV/NUV bands data affect the fitting results of both ages and metallicities much more significantly than that of the WISE W 1/W 2 band with the BC03 models. While for the galev models, the effect of the WISE W 1/W 2 band for the metallicity fitting seems comparable to that of GALEX FUV/NUV bands, but for age the effect of the W 1/W 2 band seems less crucial than that of the FUV/NUV bands. Thus we conclude that the GALEX FUV/NUV bands are more crucial for the SED-fitting of ages and metallicities, than the other bands, and the high-quality UV data (with high photometry precision) are required.

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Age and Mass Constraints for a Young Massive Cluster in M31 Based on Spectral Energy Distribution Fitting

Cited by 9 publications

References 91 publications

The Lamost Spectroscopic Survey of Star Clusters in M31. Ii. Metallicities, Ages, and Masses

The Lamost Spectroscopic Survey of Star Clusters in M31. Ii. Metallicities, Ages, and Masses

2MASS photometry and age estimation of the globular clusters in the outer halo of M31

The effects of the WISE/GALEX photometry for the SED-fitting with M31 star clusters and candidates

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