@article{han_bayesed:_2014,
	title = {{BayeSED}: {A} {General} {Approach} to {Fitting} the {Spectral} {Energy} {Distribution} of {Galaxies}},
	volume = {215},
	issn = {1538-4365},
	shorttitle = {{BayeSED}},
	url = {http://arxiv.org/abs/1408.6399},
	doi = {10.1088/0067-0049/215/1/2},
	abstract = {We present a newly developed version of BayeSED, a general Bayesian approach to the spectral energy distribution (SED) fitting of galaxies. The new BayeSED code has been systematically tested on a mock sample of galaxies. The comparison between estimated and inputted value of the parameters show that BayeSED can recover the physical parameters of galaxies reasonably well. We then applied BayeSED to interpret the SEDs of a large Ks-selected sample of galaxies in the COSMOS/UltraVISTA field with stellar population synthesis models. With the new BayeSED code, a Bayesian model comparison of stellar population synthesis models has been done for the first time. We found that the model by Bruzual \& Charlot (2003), statistically speaking, has larger Bayesian evidence than the model by Maraston (2005) for the Ks-selected sample. Besides, while setting the stellar metallicity as a free parameter obviously increases the Bayesian evidence of both models, varying the IMF has a notable effect only on the Maraston (2005) model. Meanwhile, the physical parameters estimated with BayeSED are found to be generally consistent with those obtained with the popular grid-based FAST code, while the former exhibits more natural distributions. Based on the estimated physical parameters of galaxies in the sample, we qualitatively classified the galaxies in the sample into five populations that may represent galaxies at different evolution stages or in different environments. We conclude that BayeSED could be a reliable and powerful tool for investigating the formation and evolution of galaxies from the rich multi-wavelength observations currently available. A binary version of MPI parallelized BayeSED code is publicly available at https://bitbucket.org/hanyk/bayesed.},
	number = {1},
	urldate = {2018-02-07},
	journal = {The Astrophysical Journal Supplement Series},
	author = {Han, Yunkun and Han, Zhanwen},
	month = oct,
	year = {2014},
	note = {arXiv: 1408.6399},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {2},
}

{"_id":"6Du8cDfaQzixRDBW3","bibbaseid":"han-han-bayesedageneralapproachtofittingthespectralenergydistributionofgalaxies-2014","author_short":["Han, Y.","Han, Z."],"bibdata":{"bibtype":"article","type":"article","title":"BayeSED: A General Approach to Fitting the Spectral Energy Distribution of Galaxies","volume":"215","issn":"1538-4365","shorttitle":"BayeSED","url":"http://arxiv.org/abs/1408.6399","doi":"10.1088/0067-0049/215/1/2","abstract":"We present a newly developed version of BayeSED, a general Bayesian approach to the spectral energy distribution (SED) fitting of galaxies. The new BayeSED code has been systematically tested on a mock sample of galaxies. The comparison between estimated and inputted value of the parameters show that BayeSED can recover the physical parameters of galaxies reasonably well. We then applied BayeSED to interpret the SEDs of a large Ks-selected sample of galaxies in the COSMOS/UltraVISTA field with stellar population synthesis models. With the new BayeSED code, a Bayesian model comparison of stellar population synthesis models has been done for the first time. We found that the model by Bruzual & Charlot (2003), statistically speaking, has larger Bayesian evidence than the model by Maraston (2005) for the Ks-selected sample. Besides, while setting the stellar metallicity as a free parameter obviously increases the Bayesian evidence of both models, varying the IMF has a notable effect only on the Maraston (2005) model. Meanwhile, the physical parameters estimated with BayeSED are found to be generally consistent with those obtained with the popular grid-based FAST code, while the former exhibits more natural distributions. Based on the estimated physical parameters of galaxies in the sample, we qualitatively classified the galaxies in the sample into five populations that may represent galaxies at different evolution stages or in different environments. We conclude that BayeSED could be a reliable and powerful tool for investigating the formation and evolution of galaxies from the rich multi-wavelength observations currently available. A binary version of MPI parallelized BayeSED code is publicly available at https://bitbucket.org/hanyk/bayesed.","number":"1","urldate":"2018-02-07","journal":"The Astrophysical Journal Supplement Series","author":[{"propositions":[],"lastnames":["Han"],"firstnames":["Yunkun"],"suffixes":[]},{"propositions":[],"lastnames":["Han"],"firstnames":["Zhanwen"],"suffixes":[]}],"month":"October","year":"2014","note":"arXiv: 1408.6399","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"2","bibtex":"@article{han_bayesed:_2014,\n\ttitle = {{BayeSED}: {A} {General} {Approach} to {Fitting} the {Spectral} {Energy} {Distribution} of {Galaxies}},\n\tvolume = {215},\n\tissn = {1538-4365},\n\tshorttitle = {{BayeSED}},\n\turl = {http://arxiv.org/abs/1408.6399},\n\tdoi = {10.1088/0067-0049/215/1/2},\n\tabstract = {We present a newly developed version of BayeSED, a general Bayesian approach to the spectral energy distribution (SED) fitting of galaxies. The new BayeSED code has been systematically tested on a mock sample of galaxies. The comparison between estimated and inputted value of the parameters show that BayeSED can recover the physical parameters of galaxies reasonably well. We then applied BayeSED to interpret the SEDs of a large Ks-selected sample of galaxies in the COSMOS/UltraVISTA field with stellar population synthesis models. With the new BayeSED code, a Bayesian model comparison of stellar population synthesis models has been done for the first time. We found that the model by Bruzual \\& Charlot (2003), statistically speaking, has larger Bayesian evidence than the model by Maraston (2005) for the Ks-selected sample. Besides, while setting the stellar metallicity as a free parameter obviously increases the Bayesian evidence of both models, varying the IMF has a notable effect only on the Maraston (2005) model. Meanwhile, the physical parameters estimated with BayeSED are found to be generally consistent with those obtained with the popular grid-based FAST code, while the former exhibits more natural distributions. Based on the estimated physical parameters of galaxies in the sample, we qualitatively classified the galaxies in the sample into five populations that may represent galaxies at different evolution stages or in different environments. We conclude that BayeSED could be a reliable and powerful tool for investigating the formation and evolution of galaxies from the rich multi-wavelength observations currently available. A binary version of MPI parallelized BayeSED code is publicly available at https://bitbucket.org/hanyk/bayesed.},\n\tnumber = {1},\n\turldate = {2018-02-07},\n\tjournal = {The Astrophysical Journal Supplement Series},\n\tauthor = {Han, Yunkun and Han, Zhanwen},\n\tmonth = oct,\n\tyear = {2014},\n\tnote = {arXiv: 1408.6399},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {2},\n}\n\n","author_short":["Han, Y.","Han, Z."],"key":"han_bayesed:_2014","id":"han_bayesed:_2014","bibbaseid":"han-han-bayesedageneralapproachtofittingthespectralenergydistributionofgalaxies-2014","role":"author","urls":{"Paper":"http://arxiv.org/abs/1408.6399"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["bayesed","general","approach","fitting","spectral","energy","distribution","galaxies","han","han"],"title":"BayeSED: A General Approach to Fitting the Spectral Energy Distribution of Galaxies","year":2014}