scholarly journals SEDfit: Software for Spectral Energy Distribution Fitting of Photometric Data

2012 ◽  
Vol 124 (921) ◽  
pp. 1208-1218 ◽  
Author(s):  
Marcin Sawicki
Keyword(s):  
Energy Distribution ◽  
Spectral Energy Distribution ◽  
Photometric Data ◽  
Spectral Energy ◽  
Distribution Fitting

scholarly journals Timing the earliest quenching events with a robust sample of massive quiescent galaxies at 2 < z < 5

2020 ◽  
Vol 496 (1) ◽  
pp. 695-707 ◽  
Author(s):  
A C Carnall ◽  
S Walker ◽  
R J McLure ◽  
J S Dunlop ◽  
D J McLeod ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Selection Criteria ◽  
Spectral Energy Distribution ◽  
Photometric Data ◽  
Spectral Energy ◽  
Distribution Fitting ◽  
Star Forming ◽  
Photometric Redshift ◽  
The Times ◽  
Lower Redshift

ABSTRACT We present a sample of 151 massive (M* &gt; 1010 M⊙) quiescent galaxies at 2 &lt; z &lt; 5, based on a sophisticated Bayesian spectral energy distribution fitting analysis of the CANDELS UDS and GOODS-South fields. Our sample includes a robust sub-sample of 61 objects for which we confidently exclude low-redshift and star-forming solutions. We identify 10 robust objects at z &gt; 3, of which 2 are at z &gt; 4. We report formation redshifts, demonstrating that the oldest objects formed at z &gt; 6; however, individual ages from our photometric data have significant uncertainties, typically ∼0.5 Gyr. We demonstrate that the UVJ colours of the quiescent population evolve with redshift at z &gt; 3, becoming bluer and more similar to post-starburst galaxies at lower redshift. Based upon this, we construct a model for the time evolution of quiescent galaxy UVJ colours, concluding that the oldest objects are consistent with forming the bulk of their stellar mass at z ∼ 6–7 and quenching at z ∼ 5. We report spectroscopic redshifts for two of our objects at z = 3.440 and 3.396, which exhibit extremely weak Ly α emission in ultra-deep VANDELS spectra. We calculate star formation rates based on these line fluxes, finding that these galaxies are consistent with our quiescent selection criteria, provided their Ly α escape fractions are &gt;3 and &gt;10 per cent, respectively. We finally report that our highest redshift robust object exhibits a continuum break at λ ∼ 7000 Å in a spectrum from VUDS, consistent with our photometric redshift of $z_\mathrm{phot}=4.72^{+0.06}_{-0.04}$. If confirmed as quiescent, this object would be the highest redshift known quiescent galaxy. To obtain stronger constraints on the times of the earliest quenching events, high-SNR spectroscopy must be extended to z ≳ 3 quiescent objects.

scholarly journals The stellar metallicity distribution in intermediate-latitude fields

2012 ◽  
Vol 8 (S295) ◽  
pp. 319-319
Author(s):  
Xiyan Peng ◽  
Cuihua Du ◽  
Zhenyu Wu
Keyword(s):  
Energy Distribution ◽  
Spectral Energy Distribution ◽  
Photometric Data ◽  
Spectral Energy ◽  
Galactic Centre ◽  
Fitting Method ◽  
The Galaxy ◽  
The Mean ◽  
Metallicity Distribution

AbstractBased on BATC and SDSS photometric data, we adopt the spectral energy distribution (SED) fitting method to evaluate stellar metallicities in the Galaxy. We find that the mean metallicity shifts from metal-rich to metal-poor with the increase of distance from the Galactic Centre.

scholarly journals SURVEY DESIGN FOR SPECTRAL ENERGY DISTRIBUTION FITTING: A FISHER MATRIX APPROACH

2012 ◽  
Vol 749 (1) ◽  
pp. 72 ◽  
Author(s):  
Viviana Acquaviva ◽  
Eric Gawiser ◽  
Steven J. Bickerton ◽  
Norman A. Grogin ◽  
Yicheng Guo ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Survey Design ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Matrix Approach ◽  
Distribution Fitting ◽  
Fisher Matrix

scholarly journals DUST IN THE DIFFUSE EMISSION OF THE GALACTIC PLANE: THE HERSCHEL / SPITZER SPECTRAL ENERGY DISTRIBUTION FITTING

2010 ◽  
Vol 724 (1) ◽  
pp. L44-L47 ◽  
Author(s):  
M. Compiègne ◽  
N. Flagey ◽  
A. Noriega-Crespo ◽  
P. G. Martin ◽  
J.-P. Bernard ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Galactic Plane ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Diffuse Emission ◽  
Distribution Fitting

scholarly journals MCSED: A Flexible Spectral Energy Distribution Fitting Code and Its Application to z ∼ 2 Emission-line Galaxies

2020 ◽  
Vol 899 (1) ◽  
pp. 7
Author(s):  
William P. Bowman ◽  
Gregory R. Zeimann ◽  
Gautam Nagaraj ◽  
Robin Ciardullo ◽  
Caryl Gronwall ◽  
...  
Keyword(s):  
Energy Distribution ◽  
Emission Line ◽  
Spectral Energy Distribution ◽  
Spectral Energy ◽  
Distribution Fitting ◽  
Emission Line Galaxies

scholarly journals 3D Studies of Galaxies in Compact Groups

2014 ◽  
Vol 10 (S309) ◽  
pp. 175-177
Author(s):  
Claudia Mendes de Oliveira ◽  
Sergio Torres-Flores ◽  
Philippe Amram ◽  
Henri Plana ◽  
Benoit Epinat
Keyword(s):  
Star Formation ◽  
Energy Distribution ◽  
Compact Group ◽  
Spectral Energy Distribution ◽  
Interacting Galaxies ◽  
Spectral Energy ◽  
Compact Groups ◽  
Distribution Fitting ◽  
Fabry Perot ◽  
Fisher Relation

AbstractFabry-Perot data of compact group galaxies have been used to show that the Tully-Fisher relation in any photometric band, for galaxies with vmax > 100 km/s, is very similar to that for galaxies in other less dense environments. In the low-luminosity end, however, a few compact group galaxies fall above the relation apparently because they are too bright for their mass. Here we show that if the mass is properly computed from spectral energy distribution fitting or mass modelling, for the low-luminosity galaxies, their positions in the stellar-mass or baryonic Tully-Fisher relation are what is expected for a normal Tully-Fisher relation and the outlying positions observed in the B and K Tully-Fisher relation could be explained by brightening of the low-luminosity interacting galaxies due to strong star formation or AGN activity.

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